adsabs/AstroCLIMB huggingface dataset:
Paper: Statistical Reevaluation of the Ultra-short-period Planet Classification Boundary: Smaller Planets within 1 Day, Larger Period Ratios below 2 Days
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Planets are systematically smaller in size for P ≲ 1 day and more detached from their companions for P ≲ 2 days. Pooling our USP and non-USP samples to remain agnostic to the conventional 1 day USP classification boundary, we use the permutation-based AD test to assess the level of statistical discrepancy present between the 199 systems with innermost period P1 < 3, sorted into moving bins of 30 systems each, and a non-USP control sample of the remaining 177 systems with 3 ≤ P1/days < 5 (see Section 4). The discrepancy observed in planetary size (solid red line) is rendered statistically insignificant (p > 0.05, above dashed black line) at ﹩{P}_{R}=0.9{7}_{-0.19}^{+0.25}﹩, while the analogous discrepancy in period ratio (dashed red line) disappears beyond ﹩{P}_{{ \mathcal P }}=2.0{9}_{-0.22}^{+0.16}﹩. The former value lies in substantial accord with the conventional 1 day USP classification boundary, while the latter substantiates the existence of a distinct proto-USP population with 1 ≤ P1/days < 2 (S. P. Schmidt et al. 2024). The identified cutoff periods, within their 1σ uncertainty ranges, respectively correspond to isolated, monotonic increases of ∼2–3 orders of magnitude in pR and ﹩{p}_{{ \mathcal P }}﹩, indicating that the determined values of PR and ﹩{P}_{{ \mathcal P }}﹩ are largely insensitive to the choice of critical p-value and are themselves representative of underlying transitions between astrophysical regimes (the latter point is discussed in Section 6).
Paper: Statistical Reevaluation of the Ultra-short-period Planet Classification Boundary: Smaller Planets within 1 Day, Larger Period Ratios below 2 Days
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Probability (fmiss) of an undetected innermost or second innermost planet within each USP and non-USP system. USP systems exhibit a greater likelihood of hosting an undetected companion, in accord with previous findings (e.g., J. H. Steffen & J. L. Coughlin 2016; Y. Qian & Y. Wu 2021), although this likelihood itself falls below ∼30% for vast majority of both USP and non-USP systems, qualitatively indicating that detection biases are likely of insignificant influence with regard to our primary results. A rigorous empirical investigation of this claim, which includes the calculation of fmiss, is detailed in Section 5.4: we modify our primary binning null hypothesis procedure (Section 4 and Figure 3) such that each system is subject to 1000 trials of a mock observational scheme where a randomly generated planet may be added to the inner system architecture if the planet falls below the detection threshold for the system itself. We obtain from this procedure characteristic orbital periods of ﹩{P}_{R}=0.9{2}_{-0.15}^{+0.28}﹩ day and ﹩{P}_{{ \mathcal P }}=2.1{6}_{-0.19}^{+0.19}﹩, confirming that our identified transitions in planetary size and spacing are not confounded by missing worlds or detection biases.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Comparison between constraints provided by the CRIRES+ RV data only (A), the GRAVITY KP data only (B), and the combination of both (C). The rows present in turn the visual orbit of Bb around Ba, their projected separation, the position angle of Bb around Ba, the barycentric RV of Ba, and the relative RV of Bb–Ba. The color of the lines corresponds to the mean anomaly—that is, the progress in time of the companion Bb in its orbit around Ba—with 0 marking the periastron (closest approach) and 2π marking one full orbital period. The colored dots mark the posterior values at mean times of the five GRAVITY epochs. The RV data points are plotted in black. With only the GRAVITY data, the posterior has four modes, as seen in the bottom two RV panels. Part of the multimodality comes from the usual sign ambiguity in motion toward or away from the observer from astrometric data alone, and the other is a period ambiguity caused by position-angle ambiguity in the third and fourth GRAVITY epochs. The RV-only posterior has excellent agreement with one of these four modes.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Bottom left: corner plot comparing key variables from three different models. The model with only RV data is shown in orange, the model with only GRAVITY KP data is shown in green, and the model with both GRAVITY and RV data is shown in blue. Note that while the RV data alone cannot constrain the inclination, they can when combined with a prior on the total mass of Ba + Bb adopted from G. M. Brandt et al. (2021). The KP-only posterior has four modes, one of which overlaps with one of two modes from the RV-only posterior. There is very good agreement between the RV and GRAVITY posteriors, and combining them together results in the unimodal distribution shown in blue. Top right: the same as the KP and RV series (blue) in the bottom left, with the scale adjusted to show detail. These are the results originally presented in J. W. Xuan et al. (2024). The contours correspond to 1σ and 3σ.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Outer-orbit posterior of the tight binary B around the primary A updated with new relative astrometry. The panels in the left column show the relative separation, position angle, and apparent proper motion induced by the binary. The bottom three subpanels plot the residual proper motion at the Hipparcos (“H”), Gaia (“G”), and Gaia–Hipparcos (“G-H”) epochs. The top right panel shows the projected orbit of B relative to A. The color schemes in these plots indicate the mean anomaly of each orbit draw, progressing from 0 (periastron) to 2π (a complete orbit). The bottom right panels show the RV data fit of one of the posterior samples, showing an upturn in RV around 2020. The solid color error bars indicate the data uncertainty, and the gray error bars indicate the jitter and data uncertainty added in quadrature.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: KP detection maps calculated at each epoch. Looking at the GRAVITY data alone, there are two ranges of orbital period that are equally likely. This is because the 2024 February 28 and 2024 March 29 observations cannot distinguish between two different position angles, though these locations have essentially the same separation. Thankfully, the addition of the RV data resolves this ambiguity. The maps were generated by adopting the maximum a posteriori spectral correlation, contrasts, and KP jitters per epoch.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: In-depth comparison of variable contrast model to data to aid in diagnosing the observed contrast variations. A: u–v-plane coverage at each epoch overlying the binary model visibility amplitude. B: KP data (points) and the variable contrast model (lines) vs. wavelength, separated by epoch and KP index. Notably, the first epoch, though high SNR, only marginally resolves the companion toward the second half of the epoch. This may explain why we find a higher contrast at this epoch.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: The semi-analytic correlation matrix from J. Kammerer et al. (2020) adopted in our model for closure phases (left) and projected into KPs (right). The indices run first over wavelength and then by closure-phase or KP index. The closure-phase correlation matrix on the left is rank deficient and therefore cannot be used to define a multivariate normal distribution for MCMC sampling. Projecting it onto a nonredundant KP basis solves this issue.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Comparison of orbit posteriors between the three flux models, considering the variation in either spectral contrast or variation over time.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Contrast between Bb and Ba vs. GRAVITY epoch. In this model, the contrast is averaged over wavelengths but allowed to vary over time.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Marginal distribution of spectral contrast between Bb and Ba from the “flexible contrast vs. wavelength” model.
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Mass posteriors from this work and G. M. Brandt et al. (2021). The dashed lines show the mass as determined only by the reflex motion of the primary star A. The solid blue line shows the mass as determined only by the RVs of the binary Ba and Bb. The solid black line is the combination of these two measurements (the “steady-contrast model,” to be precise), which updates the G. M. Brandt et al. (2021; gold) prior from the outer orbit with the new information from the inner orbit (blue).
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Corner plot of selected variables from the outer-orbit posterior. Despite agreeing on the secondary mass, we find substantially higher semimajor axis and lower eccentricity than T. D. Brandt et al. (2020) and G. M. Brandt et al. (2021).
Paper: On the Orbit of the Binary Brown Dwarf Companion GL229 Ba and Bb
Authors: William Thompson, Dori Blakely, Jerry W. Xuan, Alexandre Bouchard-Côté, Guillaume Bourdarot, Miguel Biron-Lattes, Trevor Campbell, Frank Eisenhauer, Thomas Henning, Markus Janson, Doug Johnstone, Jens Kammerer, Quinn Konopacky, Sylvestre Lacour, Christian Marois, Dimitri Mawet, Antoine Mérand, Jayke Samson Nguyen, Eric Nielsen, Emily Rickman, Jean-Baptiste Ruffio, Nikola Surjanovic, Jason J. Wang, 劲飞 王, Thomas Winterhalder
Figure caption: Mutual inclination between the inner (“steady-contrast” model) and outer orbits, and comparison of the orbit orientations between the systems.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Left: observed and fitted Hipparcos and Gaia proper motions of HD 73344 in R.A. (top) and decl. (bottom). The blue and red lines are models with orbital inclination smaller or larger than 90°. Right: the joint posterior distributions for the cosine term of orbital inclination ﹩\cos {I}_{d}﹩, orbital inclination Id, mass md, and semimajor axis ad of HD 73344 d from combined fitting of RV and Hipparcos–Gaia astrometric acceleration. Moving outward, the dashed lines on the corner plots correspond to 1, 2, and 3σ contours. For ﹩\cos {I}_{d}﹩ and Id, red and blues lines correspond to two peaks symmetrically positioned about 90°, which arise from the degeneracy between prograde and retrograde orbits. The orange dashed lines in the one-dimensional distribution of mass md and semimajor axis ad denote median values with 1σ interval. The graphic in the upper-right corner shows the prograde and retrograde orbits for a planet in the same orbital plane. The black arrows show the line-of-sight direction, and the blue and red arrows give the orbital axis of the planet.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: N-body simulations of the dynamical evolution of the HD 73344 system. Panel (a): the eccentricities of the three planets as a function of time. Panel (b): the orbital inclination of the three planets as a function of time. Panel (c): the mutual inclination between the two inner planets as a function of time. Panels (d)–(f): zoom-in versions of panels (a)–(c).
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: (a) The black line shows the periodogram of all RVs (except those from SOPHIE) computed using RVsearch. The blue line shows the periodogram of the SHK index from HIRES and APF observations. The red dashed line corresponds to 0.1% FAP. (b) HIRES and APF RVs vs. SHK index. (c) HIRES and APF RV residuals after removing signal from HD 73344 b and c vs. SHK index.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Left: sketch to show the mutual inclinations between two planets orbiting in the same direction (ΔI < 90°) and orbiting in opposite directions (ΔI > 90°), respectively. The gray circle and arrow show the orbit and orbital axis of the inner planet. The blue and red circles and arrows denote the orbits and orbital axes of the outer planet in two scenarios. Right: posterior distribution of mutual inclination between HD 73344 b and d.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Top: the distribution of stellar obliquity projected in the line-of-sight direction for HD 73344 b. The black dashed lines correspond to the maximum likelihood value with 1σ credible intervals. Bottom: the distribution of stellar obliquity projected in the line-of-sight direction for HD 73344 d for prograde (blue) and retrograde (gray) scenarios.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Best-fit three-planet Keplerian orbital model for HD 73344. Panel (a): HD 73344 RVs with errors (black) and their best-fit model (blue) as a function of time. Panel (b): the residuals. Panels (c)–(e): RV data and models for each planet phase-folded at the best-fit orbital period with all other planets’ signals removed.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Panels (a) and (b): TESS light curves of HD 73344 obtained in Sectors 45, 46, 71, and 72 with the modulation model at a period of 9.03 days. Panel (c): Lomb–Scargle periodogram of the detrended TESS light curves of HD 73344 using SIP (C. Hedges et al. 2020). The highest peak in the periodogram is located at 9.03 days.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: 5σ contrast curve from Keck/NIRC2 AO imaging of HD 73344. No stellar companions were detected.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Posterior distribution of stellar inclination. The dark and light shadows represent the 1 and 2σ credible regions, respectively.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: Left: the blue dots represent the raw light-curve data, while the red line indicates the fitting results. The green lines emphasize the Max. I and Max. II points within the light curves. Middle: the graph illustrates the Δmag = Max. I–Max. II distribution specifically for 338 light curves. Right: the distribution of effective temperatures.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: The blue light curve on the left was synthesized by PHOEBE, whereas the model (less massive filling), using the same input parameters, produced the orange curve. Meanwhile, the distribution shown on the right illustrates the standard deviation of the residuals between the model’s predicted light curves and PHOEBE’s synthetic curves.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: This figure serves as a visual depiction of the NN's structural framework, wherein the numerical labels correspond to the neuron count within each designated layer.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: Time evolution of radial [El/H] gradients for the OCs. The blue and red filled circles represent OCs with ages  <1 Gyr and  >1 Gyr, respectively. The blue and red lines show the corresponding linear fits for these two age bins.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: [El/H] as a function of the magnitude of the vertical distance (﹩\left|Z\right|﹩) from the Galactic plane for the clusters. Linear fits to the distribution are represented by black lines.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: AMR of OCs. The solid line represents the linear fit to the observational data.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: The vertical [El/H] gradients for the OCs. Linear fits for Z < 0 and Z >  0 are represented by blue and red lines, respectively.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: Radial elemental abundance gradients as a function of RGC for all the sample OCs (gray circles) and for clusters with more than two member stars (blue circles). The solid lines are linear regression model fits.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: Shape of radial [Fe/H] gradient in our sample clusters. The black and red lines are the linear and LOWESS fits, respectively.