adsabs/AstroCLIMB huggingface dataset:
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: Similar to Figure 18, but for Stokes V. Black contours represent V/Ipeak at 0.1%, 0.3%, and 0.5%, respectively, while red dashed contours represent V/Ipeak at −0.1%, −0.3%, and −0.5%, respectively.
Paper: I-band Asymptotic Giant Branch Stars. I. Exploring a New Standard Candle for the Extragalactic Distance Scale 
Authors: Barry F. Madore, Wendy L. Freedman, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Selection of IAGB stars in the Small Magellanic Cloud. The I-band CMD for stars in the SMC is shown in the left panel. The marginalized luminosity function of the stars with (V – I)  >  2.0 mag (black line) is shown in the right panel. The red luminosity functions are the result of changing the red color cutoff by  ±0.1 mag so as to give a visual indication of the sensitivity of the modal value to the adopted blue cutoff. The blue line is a Gaussian fit to the core of the black luminosity function having a sigma of 0.22 mag and a maximum occurring at an apparent magnitude of I = 14.37  ±  0.22 mag. 916 IAGB stars are found within 2σ of the modal magnitude, resulting in an error on the mean of 0.25/﹩\sqrt{(}915)﹩ = 0.008 mag. The dashed blue line indicates the level of the TRGB discontinuity, emphasizing the brighter 0.5 mag advantage of the IAGB over the TRGB as a distance indicator.
Paper: I-band Asymptotic Giant Branch Stars. I. Exploring a New Standard Candle for the Extragalactic Distance Scale 
Authors: Barry F. Madore, Wendy L. Freedman, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Detection and measurement of the apparent I-band magnitude of the TRGB in NGC 4258. Left panel: the CMD showing RGB stars in blue, The TRGB is marked by the two black horizontal lines at I = 25.30 mag crossing the entire figure. Middle panel: the smoothed luminosity function of the stars in the CMD to the left. Right panel: the edge-detection response (blue line) to passing an MF4 kernel (a modified Sobel filter, taken from B. F. Madore et al. 2023). The peak response marks the TRGB. The fainter red line is the unweighted fit; the blue line is the noise-weighted response. Note that the noise-weighted response is unbiased for all fluctuations; however, it noticeably suppresses false positives, which are due to Poisson fluctuations in the number counts, and enhances the contrast only for the true TRGB, as previously demonstrated in the extensive simulations of B. F. Madore et al. (2023).
Paper: I-band Asymptotic Giant Branch Stars. I. Exploring a New Standard Candle for the Extragalactic Distance Scale 
Authors: Barry F. Madore, Wendy L. Freedman, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Same as Figure 2 except that the upper panel shows the results for a color cut at (V – I) = 3.0 mag, and the lower panel shows a color cut at (V – I) = 2.0 mag. The mode of the IAGB is unchanged for the redder cut, while the mode for the bluer cut shifts fainter by only 0.04 mag. The blue horizontal line in the right half of the lower panel shows the modal value from Figure 2. The widths of the fitted Gaussian systematically change, with the redder cut being 0.18 and 0.26 mag for the bluer cut.
Paper: I-band Asymptotic Giant Branch Stars. I. Exploring a New Standard Candle for the Extragalactic Distance Scale 
Authors: Barry F. Madore, Wendy L. Freedman, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Detection and measurement of the IAGB population in NGC 4258 as marked by the circled red points in the left panel. Marginalized luminosity functions for the color-selected IAGB stars are shown in the right panel. The black line is the adopted curve fit by a Gaussian (the thick black line) centered at I = 24.65 mag, having a sigma of 0.24 mag. The red lines to either side of the adopted luminosity function are the result of shifting the blue cut off by  ±0.1 mag, so as to illustrate the effect of that choice on the adopted modal value of the IAGB luminosity.
Paper: Star Proper Motions Based on Two-epoch Observations from the SDSS and DESI Imaging Surveys
Authors: Yun-Ao Xiao, Hu Zou, Xin Xu, Lu Feng, Wei-Jian Guo, Wen-Xiong Li, Shu-Fei Liu, Zhi-Xia Shen, Gaurav Singh, Ji-Peng Sui, Jia-Li Wang, Sui-Jian Xue
Figure caption: Comparison of proper motions for 15 star clusters derived from both our and the Gaia catalogs. The left panel focuses on the comparison of ﹩{\mu }_{{\alpha }_{* }}﹩. The right panel presents the corresponding comparison for μδ. The black dashed line displays y = x. Data points marked in red represent clusters with the number of DESI−SDSS or Gaia member stars less than 100.
Paper: Searching for GEMS: TOI-5688 A b, a Low-density Giant Orbiting a High-metallicity Early M-dwarf 
Authors: Varghese Reji, Shubham Kanodia, Joe P. Ninan, Caleb I. Cañas, Jessica Libby-Roberts, Andrea S. J. Lin, Arvind F. Gupta, Tera N. Swaby, Alexander Larsen, Henry A. Kobulnicky, Philip I. Choi, Nez Evans, Sage Santomenna, Isabelle Winnick, Larry Yu, Jaime A. Alvarado-Montes, Chad F. Bender, Lia Marta Bernabó, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Samuel Halverson, Te Han, Fred Hearty, Sarah E. Logsdon, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Paul Robertson, Devendra K. Ojha, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Jason Wright
Figure caption: Plot of planet density with metallicity and equilibrium temperature of the planet. The upper plot shows the stellar metallicity-density space. The lower plot shows the equilibrium temperature-density space. The color of data points represents the radius of the planet. Both the host-star metallicity and equilibrium temperature are likely to affect the density of the planet.
Paper: Searching for GEMS: TOI-5688 A b, a Low-density Giant Orbiting a High-metallicity Early M-dwarf 
Authors: Varghese Reji, Shubham Kanodia, Joe P. Ninan, Caleb I. Cañas, Jessica Libby-Roberts, Andrea S. J. Lin, Arvind F. Gupta, Tera N. Swaby, Alexander Larsen, Henry A. Kobulnicky, Philip I. Choi, Nez Evans, Sage Santomenna, Isabelle Winnick, Larry Yu, Jaime A. Alvarado-Montes, Chad F. Bender, Lia Marta Bernabó, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Samuel Halverson, Te Han, Fred Hearty, Sarah E. Logsdon, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Paul Robertson, Devendra K. Ojha, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Jason Wright
Figure caption: (a) Series of RV measurements of TOI-5688 A with HPF (green) and NEID (red). The values are given in Table 2. The best-fitting model from the joint fit of the transit and RVs is plotted in blue, including a 16%–84% confidence interval in light blue. The bottom panel shows the residuals after subtracting the model. (b) Phase-folded RV observations at the best-fit orbital period from the joint fit from Section 4. The eccentricity was not constrained in the fit; however, the results are consistent with a circular orbit (Table 4).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.).
Paper: Searching for GEMS: TOI-5688 A b, a Low-density Giant Orbiting a High-metallicity Early M-dwarf 
Authors: Varghese Reji, Shubham Kanodia, Joe P. Ninan, Caleb I. Cañas, Jessica Libby-Roberts, Andrea S. J. Lin, Arvind F. Gupta, Tera N. Swaby, Alexander Larsen, Henry A. Kobulnicky, Philip I. Choi, Nez Evans, Sage Santomenna, Isabelle Winnick, Larry Yu, Jaime A. Alvarado-Montes, Chad F. Bender, Lia Marta Bernabó, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Samuel Halverson, Te Han, Fred Hearty, Sarah E. Logsdon, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Paul Robertson, Devendra K. Ojha, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Jason Wright
Figure caption: TESS eleanor light curves for sectors 25, 26, 40, 51, 52, 53, and 54. The first two sectors (25 and 26) have an exposure time of 30 minutes, and the rest have 10 minutes. The top panel in each figure shows the raw photometry data along with pink masks showing the transit regions. The mask is defined as t0 ± 0.25 day with t0 as the transit center. The masked data was fit using a GP model, which was then subtracted (lower panel) before fitting the transit model.
Paper: Searching for GEMS: TOI-5688 A b, a Low-density Giant Orbiting a High-metallicity Early M-dwarf 
Authors: Varghese Reji, Shubham Kanodia, Joe P. Ninan, Caleb I. Cañas, Jessica Libby-Roberts, Andrea S. J. Lin, Arvind F. Gupta, Tera N. Swaby, Alexander Larsen, Henry A. Kobulnicky, Philip I. Choi, Nez Evans, Sage Santomenna, Isabelle Winnick, Larry Yu, Jaime A. Alvarado-Montes, Chad F. Bender, Lia Marta Bernabó, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Samuel Halverson, Te Han, Fred Hearty, Sarah E. Logsdon, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Paul Robertson, Devendra K. Ojha, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Jason Wright
Figure caption: Parameter space of giant exoplanets hosted by M-dwarfs. TOI-5688 A b is marked by the green circle. Other M dwarf planets within the range of mass 95–850 M⊕ are also shown in the figure, with colors representing the stellar effective temperature. The planets around FGK-type stars are added in the background and represented by gray color along with the density contours for 0.3, 0.5, 0.8, 1.0, 1.2, and 1.5 g cm−3.
Paper: Searching for GEMS: TOI-5688 A b, a Low-density Giant Orbiting a High-metallicity Early M-dwarf 
Authors: Varghese Reji, Shubham Kanodia, Joe P. Ninan, Caleb I. Cañas, Jessica Libby-Roberts, Andrea S. J. Lin, Arvind F. Gupta, Tera N. Swaby, Alexander Larsen, Henry A. Kobulnicky, Philip I. Choi, Nez Evans, Sage Santomenna, Isabelle Winnick, Larry Yu, Jaime A. Alvarado-Montes, Chad F. Bender, Lia Marta Bernabó, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Samuel Halverson, Te Han, Fred Hearty, Sarah E. Logsdon, Suvrath Mahadevan, Michael W. McElwain, Andrew Monson, Paul Robertson, Devendra K. Ojha, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Jason Wright
Figure caption: NESSI Speckle Imaging in r’ and z’ bands in the inset 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 across. The curve shows the 5σ contrast curve for TOI-5688 A in both z and r bands. The contrast curves indicate no bright companions within 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 from the host star.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Network structure of ASC-Net: the fusion of spectral data and differentiated extended data is input into an encoder composed of three convolutional layers and three fully connected layers, and then input into a decoder composed of fully connected layers through a multi-head attention mechanism module. Three skip connections are used to improve feature extraction ability, and then the categories are output through a Softmax layer.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Endmember spectra of various categories of S-type asteroids. (Left): olivine.(Center): orthopyroxene. (Right): clinopyroxene.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Spectral counts of various types of asteroids: the horizontal axis represents the taxonomy of asteroids, and the vertical axis represents the number of spectra of such asteroids.
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: The structure of the attention mechanism: self-attention mechanism (left); multi-head self-attention mechanism (right; X. Yang et al. 2019).
Paper: Transformer-based Approach for Accurate Asteroid Spectra Taxonomy and Albedo Estimation
Authors: Yijun Tang, Yunxiao Jiang, Yuxiang Feng, Xiaoming Zhang, Xiaojun Jiang
Figure caption: Four types of spectral data augmentation display, with original spectral data (red) and expanded spectral data (blue).
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Top: RGB image of the CMZ (red: Hi-GAL column density; blue: Spitzer 8 μm; orange: CMZoom continuum). The white star represents the position of Sgr A*, while the white rectangle shows the position of the Stone MC. The bottom five panels represent the data used for analysis in this paper. From left to right: H2CO integrated map observed by the Submillimeter Array, Submillimeter Array CMZoom continuum, Chandra X-ray integrated emission from 2008 to 2017, Herschel Hi-GAL column density, and PPMAP column density. Scale bars are given in orange in the lower left corner of each panel, while the beam sizes are shown in the lower right corner as orange circles.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Top-down view of the CMZ with Sgr A* plotted at (0, 0) and parabolas following Equation (1). We consider scenarios where the X-ray flare propagated 108, 118, 146, and 213 yr ago (M. Clavel et al. 2013; E. Churazov et al. 2017; D. Chuard et al. 2018; F. Marin et al. 2023; as of 2008 January 1) with errors (shaded gray area). The circles correspond to the line-of-sight distance of the Stone MC given the different ages of the events.
Paper: Utilizing Machine Learning to Predict Host Stars and the Key Elemental Abundances of Small Planets
Authors: Amílcar R. Torres-Quijano, Natalie R. Hinkel, Caleb H. Wheeler, Patrick A. Young, Luan Ghezzi, Augusto P. Baldo
Figure caption: Feature importance plots obtained for the ensembles in Experiment 1 (small planets). Because the PlanetPrediction algorithm performs thousands of iterations, during which the feature importance scores may vary, we have employed a color-coding and pattern schema to identify variations in feature importance scores. Blue coloration denotes that a particular element did not have any variations in importance score across initializations during an ensemble run. In contrast, colors other than blue indicate that those elements varied in feature importance. The hatching patterns within panels (c) and (d) indicate additional smaller (subgroup) variations that occurred within the ensembles.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Predictions of isochrones for two clusters NGC 2184 (left panel) and the dwarf galaxy Bootes I (right panel) from this work (red points) and the literature: T. Cantat-Gaudin & F. Anders (2020; blue points), W. S. Dias et al. (2021; purple points), E. L. Hunt & S. Reffert (2023; green points), and L. Cavallo et al. (2024; orange points). With filled black dots we plot the members of the clusters retrieved by this work, and with empty black dots are plotted those of the above literature.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Comparison of parameters for clusters that we have in common with four pieces of recent literature: T. Cantat-Gaudin & F. Anders (2020; top row); W. S. Dias et al. (2021; second row); E. L. Hunt & S. Reffert (2023; third row); L. Cavallo et al. (2024; bottom row). In the top left corners is reported the value of the CCC.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Example of a cluster: Alessi 5. The left panel shows the spatial distribution and density profiles of cluster member stars. The three colored circles—red, cyan, and yellow—represent the different radii: rh, rt, and re, respectively. The center panel displays the RDPs (red dots) of the cluster members, with the red and blue lines representing the fitted ρ(r) and F(r), respectively. The right panel shows the RDP fit in logarithmic coordinates.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Left panel: a synthetic CMD of Alessi 62, with single member stars represented by colored dots and binary star members by crosses. The color bar indicates the mass distribution of the stars. Right panel: the mass distributions of the primary (violet) and companion (pink) stars are displayed.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Examples of the CMD and isochrone fitting. The blue dots are the observed CMDs, and the red dots are the best-fitting isochrones.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Galactic orbits obtained from the three examples of NGC 2682, 2477, and 104 using galpy. The starting point of each orbit is marked by a blue dot, while the present position is denoted by a red dot. The center of the Galaxy is represented by a black dot, and the Sun is depicted by a red circle with a dot at its center.
Paper: Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Xingyin Wei, Jing Chen, Su Zhang, Feilong He, Yunbo Zhao, Xuran He, Yongjie Fang, Xinhao Chen, Hao Yang
Figure caption: Comparison of structure parameters derived from this study with those from the literature work of E. L. Hunt & S. Reffert (2024).
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: (a) The ∥ chJWL vs. V CMD of NGC 2257 RGB stars. (b) Same as panel (a), but for ∥ chJWL. (c) The (∥ chJWL − ∥ cnJWL) distribution of the NGC 2257 RGB stars. The blue and red plus signs denote the FG and SG RGB stars, respectively, in NGC 2257 returned from our EM estimator. (d) The histogram for the (∥ chJWL − ∥ cnJWL) distribution of the NGC 2257 RGB stars. The blue and red lines denote the FG and SG distributions, respectively, returned from our EM estimator, while the gray line is for all the stars. (e) Plot of ∥ chJWL vs. ∥ cnJWL of NGC 2257 RGB stars, showing a ∥ chJWL–∥ cnJWL anticorrelation, a surrogate of the C–N anticorrelation.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: A plot of Teff vs. ﹩\mathrm{log}\,g﹩ for NGC 2257 RGB stars from our evolutionary populational model (black circles). The blue open circles denote the stellar parameters of RGB stars derived by A. Mucciarelli et al. (2010). The thick green and orange lines are for the BaSTI model RGB sequence for [Fe/H] = −1.90 and −1.70 dex, respectively (A. Pietrinferni et al. 2021). The black plus sign denotes the location of the observed RGB tip of NGC 2257 (V ∼ 16.5 mag) for [Fe/H] = −1.90 dex.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: Plots of  by5 vs. V CMDs and differential LFs. The blue and red lines are LFs of the FG and SG populations, respectively, while the green lines are for the LF of all the stars. We also show the RGBB V magnitudes of each population with solid gray lines, while the dotted green lines denote the RGBB V magnitude from all stars. Note that the by5 is defined to be by5 = 5 × (b − y) − 2.25 for the clarity of the figure.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: A plot of d[C/Fe]/MV vs. [Fe/H] of NGC 2257 and four Galactic GCs from our previous study (J.-W. Lee 2023b). The blue and red colors denote the FG and SG, respectively. The green line shows a linear regression, while the gray solid and dashed lines denote 95% confidence and predicted intervals, respectively.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: The CRDs and populational number ratios of the FG (blue) and SG (red) populations in NGC 2257. The horizontal solid line denotes the mean FG fraction, while the dashed lines denote the 1σ error of the mean. The blue and red filled squares with error bars indicate the FG and SG populational number ratios, respectively, with a radial bin size of 30″. The gray vertical lines denote the core and half-mass radii (B. Lanzoni et al. 2019).
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: The hkJWL,0 vs. MV CMDs of NGC 2257 RGB stars, assuming (m − M)0 = 18.376 mag and E(B − V) = 0.038 mag for NGC 2257. We also show fiducial sequences of the eight Galactic GCs with various metallicities from our previous studies.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: The [Fe/H]hk histograms for the FG (blue solid line) and SG (red solid line shaded with gray) in NGC 2257. The small vertical lines denote the locations of the 5th and 95th percentiles of [Fe/H]hk distributions for each population.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: The [Fe/H]hk, [C/Fe]ch, and [N/Fe]﹩{}_{{cn}}﹩ against V magnitude.