adsabs/AstroCLIMB huggingface dataset:
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Correlation between A.S.A.D and STARLIGHT age values obtained in this work (top), literature and A.S.A.D (middle) and STARLIGHT (bottom). Errors bars are also indicated. The blue line is the ±σ shift and the orange line is the ±3σ shift.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: The observed and reddening-corrected (with E(B − V) = 0.22) spectra of NGC 1718, in black and pink, respectively, along with the best matching models. A.S.A.D model, with one SSP, in green, and STARLIGHT synthetic spectrum as combination of 6 SSPs, in blue.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: DSS images for the star clusters sample (6﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 × 6﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5). From upper left to bottom right: NGC 1711, NGC 1718, NGC 1801, NGC 1806, NGC 1818, NGC 1849, NGC 1866, NGC 1916, SL 505, NGC 2100, and NGC 2136 and NGC 2137. The observed regions are indicated in yellow, showing all slit positions (width = 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩0  length = 5﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5). North, east (black), and the zenith (red) direction are indicated in each panel.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Correlation between A.S.A.D and STARLIGHT age values obtained using a range of metallicities and the fixed Z = 0.008. The bottom panel presents A.S.A.D new values vs. literature ones. Errors bars are also indicated. The blue line is the ±σ shift and the orange line is the ±3σ shift.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Comparison between A.S.A.D and STARLIGHT age values obtained in this work with literature refereed in Table 2. Errors bars are also indicated.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Correlation between A.S.A.D and STARLIGHT age values obtained in this work (top), literature and STARLIGHT (middle), using a range of metallicities and fixed ones. Errors bars are also indicated. The blue line is the ±σ shift and the orange line is the ±3σ shift.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Normalized reddening-corrected spectrum using A.S.A.D. (left panels) and observed normalized spectrum using STARLIGHT (right panels) in black, and the best matching models fit in blue. The residual flux is presented in green. The dotted lines are at ±3σ. The percentage mean (﹩\overline{{\rm{\Delta }}}﹩) is indicated for each cluster.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Surface plots of age reddening for each star cluster. From top left to bottom right: NGC 1866, NGC 1916, SL 505, NGC 2100, NGC 2136, and NGC 2137.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Surface plots of age reddening for each star cluster. From top left to bottom right: NGC 1711, NGC 1718, NGC 1801, NGC 1806, NGC 1818, and NGC 1849.
Paper: Ages of Large Magellanic Cloud Star Clusters with Gemini Multi-Object Spectrograph Integrated Spectroscopy: Systematic Comparison of Available Tools
Authors: Martina I. Tapia-Reina, Randa Asa'd, Andrea V. Ahumada, Carlos Gonzalo Díaz
Figure caption: Continued from Figure 10.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: Top panel: the fading function as defined in Equation (12), representing the fraction of observed point sources as a function of PSF magnitude. The different lines represent the effect of the variation of the peak detection efficiency F and the width parameter w on the shape of the function. The 5σ limiting magnitude at the source location is marked in gray (m5σ = 24.5). Bottom panel: a histogram showing detection probability of 10,000 point sources passed through Sorcha’s fading function filter, with the actual calculated detection probability from Equation (12) overplotted as a solid line. Here, F  = 1.0, w  = 0.1, and m5σ = 24.5, and the binsize is 0.04 mag.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: The LSSTCam field of view (FOV). The overplotted circles show the recommended default search area radius (including buffer) used in Sorcha’s ephemeris generation stage (gray dashed line); the 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩06 radius circle encompasses all of the CCD detectors (blue dashed–dotted line); and the 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩75 radius circles contains 90% of LSSTCam detector area (pink solid line).
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: Left panel: the trailing losses for different values of the seeing θ, shown as a function of the object’s on-sky velocity v, given in degrees per day on the bottom axis and pixels per 30 s visit on the upper axis. Right panel: a zoomed-in version of the left panel for low v. Vertical lines represent the thresholds for typical on-sky motions of a TNO, a Jupiter Trojan, and inner and outer main-belt asteroids (MBAs; (J. X. Luu & D. Jewitt 1988, Equation (1)).
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: The effect of the full camera footprint filter on a selection of 100,000 random synthetic sources. Left panel: original sources, distributed over a circular FOV of radius 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1. Right panel: the same sources after running Sorcha’s full camera footprint filter. The shape of the LSSTCam detector footprint can be seen with the loss of detections in the raft and chip gaps.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: The effects of vignetting on the 5σ limiting magnitude for a randomized series of points on a circular FOV in the LSSTCam focal plane. Locations farther from the center of the FOV have shallower depths. The LSSTCam detector footprint is also plotted. The center of this example pointing has a limiting magnitude of 24.071.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: Histogram of differences in R.A. (left panel), decl. (center panel), and trailed source magnitudes (right panel) between Sorcha-derived values and an independent verification using JPL Horizons. The red curves show 2010 TU149, an MBA, while the blue curves show 2011 OB60, a TNO.
Paper: Sorcha: A Solar System Survey Simulator for the Legacy Survey of Space and Time
Authors: Stephanie R. Merritt, Grigori Fedorets, Megan E. Schwamb, Samuel Cornwall, Pedro H. Bernardinelli, Mario Jurić, Matthew J. Holman, Jacob A. Kurlander, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Joseph Murtagh, R. Lynne Jones, Peter Yoachim, Ryan R. Lyttle, Michael S. P. Kelley, Joachim Moeyens, Kathleen Kiker, Shantanu P. Naidu, Colin Snodgrass, Shannon M. Matthews, Colin Orion Chandler
Figure caption: A cartoon schematic of tracklet creation and the linking process for the Rubin Solar System Processing Pipeline (SSP).
Paper: An Hα Cloud in the H I Tail: Recent Star Formation in the Outskirts of NGC 4258 Revealed by Nanshan 1 m Telescope
Authors: Cheng Cheng, Jia-Sheng Huang, Peng Wei, Ali Esamdin, Guojie Feng, Zhi-Xiang Zhang, Haojing Yan, Wei Du, Pei Zuo, Zijian Li, Gustavo Orellana-González, Letian Wang, Yong Wang, Abdusamatjan Iskandar, Shahidin Yaqup
Figure caption: Right panel: false-color composite of the Nanshan 1 m Hα narrowband image (red), DECaLS R (green), and G (blue) band images (﹩2{8}^{{\prime} }\times 2{8}^{{\prime} }﹩; image top is north and left is east). We make use of the ASINH stretch to highlight the Hα emission in the galaxy center and galactic disk, while the Hα emission at the extended region is suppressed. We overplot the H I flux contours from the H I moment 0 image produced by HALOGAS project. The contours start from 0.01 Jy Beam−1 km s−1, and the H I data beam is shown in he lower-left corner with white ellipse. The detected Hα emitter locate in the H I tail and highlighted by a red box (﹩{2}^{{\prime} }\times {2}^{{\prime} }﹩). A zoomed-in version of which is shown in the left panel: color image with Hα (red), R (green), and G (blue), centered at R.A. = 12:19:33.3821, decl. = +47:23:05.509 (J2000). To highlight the H I map in the tail, we produce the H I moment 0 map by integrating the data cube along the velocity axis within 405–459 km s−1, and shown in white contours with H I column density [5, 10, 15, 20, . . . ] × 6.4 × 1020 cm−2. The complete moment 0 map for the H I tail is shown in Figure 6. The white hatched ellipse at the lower-left corner represents the synthesized beam.
Paper: An Hα Cloud in the H I Tail: Recent Star Formation in the Outskirts of NGC 4258 Revealed by Nanshan 1 m Telescope
Authors: Cheng Cheng, Jia-Sheng Huang, Peng Wei, Ali Esamdin, Guojie Feng, Zhi-Xiang Zhang, Haojing Yan, Wei Du, Pei Zuo, Zijian Li, Gustavo Orellana-González, Letian Wang, Yong Wang, Abdusamatjan Iskandar, Shahidin Yaqup
Figure caption: Top-right panel: HST color image with F555W (blue color), F814W (red color) bands, overplotted with the H I contour in white color and Hα contours in red. The image size is ﹩{2}^{{\prime} }\times {2}^{{\prime} }﹩. The H I moment 0 map is derived from 405 to 459 km s−1, which is optimized by the H I emission in the H I knots in the H I tail. The green box is the central region (11″ × 11″) of the Hα emitter, and zoom in at the top-left panel. Lower-left panel: same image as top-left panel, with F555W magnitude denoted. Lower panels: same image as the top-left panel, with the F555W AB magnitude denoted in lower-left panel and the F555W − F814W color denoted in lower-right panel. The Hα emitter region includes targets with F555W about 25–26 AB mag, and F555W − F814W ≲ 0, indicating a hot massive stellar population. The crowded blue targets in the Hα region implies the recent star-formation activity.
Paper: An Hα Cloud in the H I Tail: Recent Star Formation in the Outskirts of NGC 4258 Revealed by Nanshan 1 m Telescope
Authors: Cheng Cheng, Jia-Sheng Huang, Peng Wei, Ali Esamdin, Guojie Feng, Zhi-Xiang Zhang, Haojing Yan, Wei Du, Pei Zuo, Zijian Li, Gustavo Orellana-González, Letian Wang, Yong Wang, Abdusamatjan Iskandar, Shahidin Yaqup
Figure caption: Teff and NUV − R color (top panel), F555W − F814W color (bottom panel) for stars with ﹩{\mathrm{log}}\,{\rm{g}}\,[{\rm{cm}}\,{{\rm{s}}}^{-2}]=2.5﹩ and 3. So the typical Teff for a star with F555W − F814W lower than −0.5 should be above 15,000 K. The Hα emitter is not detected in the DECaLS R-band image, with an R-band magnitude fainter than 23 (depending on the photometric aperture). Then the upper limit on the NUV − R color is lower than −2, indicating the presence of a young, massive stellar population.
Paper: An Hα Cloud in the H I Tail: Recent Star Formation in the Outskirts of NGC 4258 Revealed by Nanshan 1 m Telescope
Authors: Cheng Cheng, Jia-Sheng Huang, Peng Wei, Ali Esamdin, Guojie Feng, Zhi-Xiang Zhang, Haojing Yan, Wei Du, Pei Zuo, Zijian Li, Gustavo Orellana-González, Letian Wang, Yong Wang, Abdusamatjan Iskandar, Shahidin Yaqup
Figure caption: Multiwavelength stamp images in GALEX/FUV, GALEX/NUV, Hα narrowband filter, DECaLS/G/R/Z, HST/F555W, and HST/F814W bands, centered on the coordinate of the Hα emitter. The size of each image is 50″ × 50″. The depth of the DECaLS images are about 24 AB mag, and the Hα emitter in G band is only marginally detected. The images are centered at R.A. = 12:19:33.3821, decl. = +47:23:05.509 (J2000).
Paper: An Hα Cloud in the H I Tail: Recent Star Formation in the Outskirts of NGC 4258 Revealed by Nanshan 1 m Telescope
Authors: Cheng Cheng, Jia-Sheng Huang, Peng Wei, Ali Esamdin, Guojie Feng, Zhi-Xiang Zhang, Haojing Yan, Wei Du, Pei Zuo, Zijian Li, Gustavo Orellana-González, Letian Wang, Yong Wang, Abdusamatjan Iskandar, Shahidin Yaqup
Figure caption: HST color image with wider field of view. The white contours are the H I moment0 flux. The cyan dots are the targets with −1 < F555W − F814W < −0.5 and F555W < 25.5, which align with the H I distribution.
Paper: Spectroscopic Orbits of Subsystems in Multiple Stars. XI
Authors: Andrei Tokovinin
Figure caption: Spectroscopic orbit of HIP 49442 Ab1,Ab2 (top, motion in the orbit of Aa,Ab is subtracted) and two representative CCFs of star A recorded in 2018 and 2022.
Paper: An Hα Cloud in the H I Tail: Recent Star Formation in the Outskirts of NGC 4258 Revealed by Nanshan 1 m Telescope
Authors: Cheng Cheng, Jia-Sheng Huang, Peng Wei, Ali Esamdin, Guojie Feng, Zhi-Xiang Zhang, Haojing Yan, Wei Du, Pei Zuo, Zijian Li, Gustavo Orellana-González, Letian Wang, Yong Wang, Abdusamatjan Iskandar, Shahidin Yaqup
Figure caption: FUV − NUV vs. NUV − R (left panel) and NUV − F555W (right panel) color for stars with ﹩{\mathrm{log}}\,{\rm{g}}\,[{\rm{cm}}\,{{\rm{s}}}^{-2}]=2.5﹩ and 3, and Teff > 15,000 as in Figure A1.
Paper: An Hα Cloud in the H I Tail: Recent Star Formation in the Outskirts of NGC 4258 Revealed by Nanshan 1 m Telescope
Authors: Cheng Cheng, Jia-Sheng Huang, Peng Wei, Ali Esamdin, Guojie Feng, Zhi-Xiang Zhang, Haojing Yan, Wei Du, Pei Zuo, Zijian Li, Gustavo Orellana-González, Letian Wang, Yong Wang, Abdusamatjan Iskandar, Shahidin Yaqup
Figure caption: H I spectrum of the Hα emitter region. The H I integrated flux is 0.12 ± 0.01 Jy km s−1, corresponding to a H I mass of 1.7 ± 0.2 × 106 M⊙.
Paper: Exploring Giant Barium Stars:12C/13C Ratio and Elemental Abundances of Carbon, Nitrogen, and Oxygen 
Authors: M. P. Roriz, N. A. Drake, N. Holanda, M. Lugaro, B. Cseh, S. Junqueira, C. B. Pereira
Figure caption: Carbon (top) and nitrogen (bottom) abundance ratios to Fe derived for the program stars (gray dots) as a function of metallicity. Typical error bars are shown in the top right side of the panels. The lines outline the average [C/Fe] and [N/Fe] ratios observed in our sample of Ba giants (blue solid line), normal field giants (red solid line), and normal field dwarfs (red dashed line). The error bars in the blue lines represent the standard deviations of the mean values observed in each metallicity bin. The shaded red areas reflect the standard deviations of the literature data for dwarf and giant normal stars. Specifically for nitrogen abundances in normal dwarfs with [Fe/H] > −0.70 dex, we have considered the homogeneous data of Y. Takeda (2023). The stars BD+09°2384, HD 107541, and HD 219116 are identified as black dots (see text). For comparison purposes, abundance data observed in Ba dwarfs (yellow dots) are also plotted in this figure; data were taken from M. P. Roriz et al. (2024a, and references therein).
Paper: Exploring Giant Barium Stars:12C/13C Ratio and Elemental Abundances of Carbon, Nitrogen, and Oxygen 
Authors: M. P. Roriz, N. A. Drake, N. Holanda, M. Lugaro, B. Cseh, S. Junqueira, C. B. Pereira
Figure caption: Panel (a): ﹩\mathrm{log}\,\epsilon ({\rm{C}}+{\rm{N}})﹩ vs. [Fe/H]; panel (b): C/O ratios vs. [Fe/H]; panel (c): ﹩\mathrm{log}\,({\rm{C}}/{\rm{N}})﹩ vs. ﹩\mathrm{log}\,({\rm{O}}/{\rm{N}})﹩; panel (d): 12C/13C ratios vs. [Fe/H]. The respective solar values are marked by the ⊙ symbol. As in Figure 3, gray dots are data for the Ba giants of this study and yellow dots are data for Ba dwarfs. The curves outline the average trends observed for the program stars (blue solid line), normal giants (red solid line), and normal dwarfs (red dashed line). The shaded red areas reflect the standard deviations of the literature data for dwarf and giant normal stars. The stars HD 107541 (1), HD 66291 (2), HD 39778 (3), HD 219116 (4), and BD+09° 2384 (5), mentioned in the text, are plotted as black dots. HD 26 is shown as a green square. In panel (a), the black straight line represents the solar scaled C+N abundance. In panel (d), data for which just lower limits were estimated are not shown, except for HD 107541, HD 66291, and HD 39778. In this figure, crosses represent data for normal giants, taken from R. E. Luck & U. Heiter (2007) and Y. Takeda et al. (2019, just abundances labeled as “reliable”). Additionally, data are shown for symbiotic stars (cyan dots, C. Gałan et al. 2016, 2017), classical CH stars (magenta dots, A. D. Vanture 1992; C. B. Pereira & N. A. Drake 2009; C. B. Pereira et al. 2012b; A. Goswami et al. 2016; M. Purandardas et al. 2019), and post-AGB stars (blue diamonds, H. Van Winckel & M. Reyniers 2000; M. Reyniers et al. 2004; K. De Smedt et al. 2012, 2015, 2016; E. van Aarle et al. 2013).
Paper: Exploring Giant Barium Stars:12C/13C Ratio and Elemental Abundances of Carbon, Nitrogen, and Oxygen 
Authors: M. P. Roriz, N. A. Drake, N. Holanda, M. Lugaro, B. Cseh, S. Junqueira, C. B. Pereira
Figure caption: [C/Fe], [N/Fe], and C/O ratios (top, middle, and bottom panels, respectively) as a function of the average s-process abundance, [s/Fe]. The observational data set (dots) was grouped within different metallicity ranges, as identified by the legend shown in the top panel. Some outlier stars are also identified. Typical error bars of these quantities are also drawn. The black straight lines are linear fits of the data. For comparison, data for normal field giants (crosses), taken from R. E. Luck & U. Heiter (2007), are plotted in these panels.
Paper: Exploring Giant Barium Stars:12C/13C Ratio and Elemental Abundances of Carbon, Nitrogen, and Oxygen 
Authors: M. P. Roriz, N. A. Drake, N. Holanda, M. Lugaro, B. Cseh, S. Junqueira, C. B. Pereira
Figure caption: Expected evolution (dashed curves) of the photospheric abundances of carbon and nitrogen, as the star leaves the main sequence and becomes a red giant. For different metallicity regimes, identified by colors in this figure and labeled in the curves, these tracks take into account only mixing due to FDU, which keep constant the C + N abundances. In this plot, the dots represent the mean C and N abundances observed in our targets, computed in bins of 0.20 dex in metallicity, centered on the metallicity regimes labeled in the curves. Error bars represent the standard deviation of the mean. The black straight line represents the solar C and N abundances scaled to metallicity. In general, the observational data present an offset from the track where they were expected to lie (see text for more explanations). The solar values are marked by the symbol ⊙.
Paper: Exploring Giant Barium Stars:12C/13C Ratio and Elemental Abundances of Carbon, Nitrogen, and Oxygen 
Authors: M. P. Roriz, N. A. Drake, N. Holanda, M. Lugaro, B. Cseh, S. Junqueira, C. B. Pereira
Figure caption: Observed average [O/Fe] ratios (blue dots) for targets selected from the program stars; these objects are representative within each bin of metallicity and cover the entire interval considered in this work, and the error bars represent the standard deviations. The black curve comes from the average [O/Fe] values reported by J. Meléndez & B. Barbuy (2002), and the shaded area outlines their standard deviations. Data for normal giants (crosses), taken from R. E. Luck & U. Heiter (2007) and Y. Takeda et al. (2019), are also plotted on this diagram.
Paper: Exploring Giant Barium Stars:12C/13C Ratio and Elemental Abundances of Carbon, Nitrogen, and Oxygen 
Authors: M. P. Roriz, N. A. Drake, N. Holanda, M. Lugaro, B. Cseh, S. Junqueira, C. B. Pereira
Figure caption: Observed (dots) and synthetic (solid lines) spectra around the spectral regions of the C2 molecular band at 5635 Å  (top panel) and CN absorption features at 8000 Å  (bottom panel) for HD 107541. The carbon and nitrogen abundances that provide the best fits (blue lines) are indicated in the panels. The shaded blue areas show the effects in changing the carbon and nitrogen abundances around the adopted values. The red lines show spectral synthesis without contribution of the C2 and CN molecules.