adsabs/AstroCLIMB huggingface dataset:
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) A plot of [C/Fe] vs. [N/Fe] for all RGB stars in NGC 2257. (b) A plot of [C/Fe] vs. [N/Fe] for all RGB stars fainter than RGBBs.
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: Top: a plot of ΔWCF336W,F438W,F814W vs. NFG/Ntot. The green filled boxes denote the in situ Galactic GCs, the orange filled circles denote the ex situ Galactic GCs, and the blue filled diamonds denote the young MC GCs. NGC 2257 is shown with a big red diamond. The thick dark-green line denotes the linear regression from the normal Galactic GCs (both in situ and ex situ), while the solid and dashed gray lines are for 95% confidence and predicted intervals, respectively. The thin green and orange solid lines show a linear regression for in situ and ex situ Galactic GCs, respectively, both of which are similar. Bottom: a plot of ΔWCF336W,F438W,F814W vs. NFG/Ntot for metal-complex Galactic GCs (red filled circles). The green line shows a linear regression of the metal-complex GCs, 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: Plots of [Fe/H] vs. σ[Fe/H], σ[C/Fe], σ[N/Fe], and σ[C+N/Fe] for NGC 2257 (red filled circle), four Galactic normal GCs (open circles), and three metal-complex GCs (gray filled circles). The thick green lines denotes the linear regressions of the four Galactic normal GCs, while the thick gray and dashed gray lines denote the 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: Plots of Δσ[C,N/Fe] vs. NFG/Ntot for four Galactic normal GCs. The green lines show linear regressions, while the gray solid and dashed lines denote 95% confidence and predicted intervals, respectively. The red filled circles denote NGC 2257, which is in good agreement with Galactic normal GCs.
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: Same as Figure 14, but for ﹩\mathrm{log}M/{M}_{\odot }﹩ vs. Δσ[Fe/H], Δσ[C/Fe], Δσ[N/Fe], and Δσ[C+N/Fe].
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 Δσ[C,N/Fe] vs. ΔWCF336W,F438W,F814W of four Galactic normal GCs from Figure 16. The red, blue, and orange open stars denote the predicted ΔWCF336W,F438W,F814W of NGC 2257.
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 ΔWCF336W,F438W,F814W vs. ﹩\mathrm{log}M/{M}_{\odot }﹩ vs. NFG/Ntot.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: GLS periodogram of RVs, residual RVs, window function, cross-correlation function (CCF) FWHM, and bisector inverse slope (BIS) are shown in panels 1–5 (top to bottom), respectively. The vertical pink line marks the most significant period (5.832 ± 0.010 days) found in the RVs, which is consistent with the period found by TESS. The rotational period of the star (9.29 days) is marked by the vertical brown dashed line. FAP levels of 0.1%, 1.0%, and 10.0% are indicated by horizontal dashed lines in blue, orange, and green, respectively.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: Mass–radius diagram of known transiting exoplanets with mass and radius constraints better than 20%, and equilibrium temperatures (Teq) between 500 and 2000 K. The sample is drawn from the TEPCat catalog (J. Southworth 2011). The light pink region highlights the sub-Saturn class, while the black dashed line indicates the iso-density curve for ρP = 1.62. The solid curves in red, orange, green, and blue represent the mass–radius relationship for pure iron, pure silicates, pure high-pressure ice (L. Zeng et al. 2021), and a pure H2 core composition (A. Becker et al. 2014), respectively. The solar system planets are shown as black dots.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: Density–period diagram of super-Neptunes and sub-Saturns with masses and radii constrained to a precision better than 20%. Planets in the savanna show low densities, typically below 1 g cm−3, while planets in the ridge show densities as high as 1.5–2.0 g cm−3 (A. Castro-González et al. 2024b). Data sourced from the NASA Exoplanet Archive.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: TOI-6038 A b in a period–radius diagram of close-in exoplanets with radii constrained to a precision better than 20%. The boundaries of the Neptunian desert, ridge, and savanna (V. Castro-González et al. 2024a) are indicated with black dashed lines. The data were collected from the NASA Exoplanet Archive (R. L. Akeson et al. 2013).
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: RVs of TOI-6038 A observed with PARAS-2 are plotted as black dots over time (left). Phase-folded RVs are shown on the right. The best-fit RV model from EF2 is represented by the solid pink line, with the residual RVs displayed in the respective lower panels.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: SED of TOI-6038 A, with red symbols representing the observed photometric measurements and horizontal bars indicating the effective width of the passbands. The blue points represent the model fluxes, and the residuals are displayed in the lower panel.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: Corner plot showing the covariances among the fitted parameters from EF2 for the high-mass solution. The inner and outer contours around the median denote the 68% and 95% confidence intervals, respectively.
Paper: TOI-6038 A b: A Dense Sub-Saturn in the Transition Regime between the Neptunian Ridge and Savanna
Authors: Sanjay Baliwal, Rishikesh Sharma, Abhijit Chakraborty, K. J. Nikitha, A. Castro-González, Hareesh G. Bhaskar, Akanksha Khandelwal, David W. Latham, Allyson Bieryla, Vincent Bourrier, Neelam J. S. S. V. Prasad, Kapil K. Bharadwaj, Kevikumar A. Lad, Ashirbad Nayak, Vishal Joshi, Jason D. Eastman
Figure caption: MIST evolutionary track for TOI-6038 A shown as a solid black line. The black point indicates the Teff and ﹩\mathrm{log}\,g﹩, while the red asterisk denotes the current age of TOI-6038 A.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Quick-reference chart for our classification of planetary system architectures, with representative model systems for each category. Each row corresponds to one planetary system, with the horizontal spacing corresponding to orbital period on a log scale and the point sizes corresponding to planet size. The colors correspond to planet type, as described in Section 2.3: Jupiters (>6 R⊕; red), Neptunes (3.5–6 R⊕; gold), sub-Neptunes (1.75–3.5 R⊕; blue), and Earths (<1.75 R⊕; green). (However, the exact composition of non-Jupiters in this figure is arbitrary.) This format is used for all plots of planetary system architectures throughout this paper. Framework summary: each system is divided into inner and outer planets (if both are detected). Systems with N ≥ 3 inner planets are classified based on whether their inner planets include any Jupiters, and whether (and, if so, where) their inner planets include large gaps with a period ratio >5. Other dynamical features are addressed separately from the overall classification system (see Section 6).
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Scatter plot and histograms of two-planet systems by mass ratio vs. inner-planet mass, divided into Jupiter pairs (red) Jupiter and non-Jupiter pairs (lavender), and non-Jupiter pairs (blue, here representing all types of non-Jupiters). The overlaps between the color-coded regions (defined by planet size) are due to the differences in assigning Jupiter status by radius rather than mass, when possible. Systems with unusually low mass ratios (smaller outer planets) are highlighted.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: The same as Figure 3 for period ratio vs. inner-planet period. (Note that the color-coded regions defined by planet size overlap strongly in period space.) Jupiters show more systems with longer periods and larger period ratios. The outliers to the right of the plot correspond to directly imaged systems.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Cumulative distributions of confirmed exoplanets with period, comparing total numbers of planets (dashed) to those in single-planet systems (solid), according to the same color scheme as in Figure 1. Hot Jupiters show far fewer companions than other planet types, as illustrated by the near-coincidence of the two Jupiter distributions at <10 days.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of directly imaged multiplanet systems, using the same format as Figure 1. While not constituting a separate category of systems themselves, direct imaging is sensitive to planets at very wide separations, so these systems are dramatic outliers from the rest of the currently observed population. All known directly imaged planets are Jupiters.
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: Comparative analysis of Stokes I parameters across various observations in inner and outer beams of the FAST Telescope. Parameters include σ1, the relative beam efficiency, beam size, position angle, ϕdif, and Pslb/Pbeam. Inner beams: M02–M07; outer beams: M08–M19. Data points from 2022, 2021, and 2020 are denoted by red circles, blue plus signs, and black squares, respectively. The red solid, black dashed, and blue dashed–dotted lines indicate the average values of the corresponding parameters across all observations, respectively. In panel (d), the black solid and black dashed lines represent the linear fitting results of the position angle distribution for the outer and inner beams, respectively.
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: Top: Mapping of Stokes Q, U, and V for the central beam across different observations. Contours (black solid lines) represent the fractional polarization Q/Ipeak, U/Ipeak, V/Ipeak at 0.1%, 0.04%, 0.02%, respectively, while contours (red dashed lines) represent the fractional polarization Q/Ipeak, U/Ipeak, V/Ipeak at −0.1%, −0.02%, −0.01%, respectively. The colorbar is marked with the fractional polarization relative to the peak of Stokes I from the central beam, denoted as Ipeak% (64.44 K, 67.50 K, and 28.85 K for data observed in 2020, 2021, and 2022, respectively). For the data observed in the same year, the colorbar range for Stokes U and V is kept consistent for comparison purposes. Bottom: Simulated Stokes Q, U, and V patterns of the central beam.
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: Stokes Q mapping of J1407+2827 for the 19 beams near 1420 MHz. To compare with the simulated beam patterns, the mapping data have been mirror-symmetrized. Black solid contours represent Q/Ipeak at 0.4%, while red dashed contours represent Q/Ipeak at −0.4%. The blank areas in the outer beams are outside the scanning region.
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: Stokes U mapping of J1407+2827 for the 19 beams near 1420 MHz. To compare with the simulated beam patterns, the mapping data have been mirror-symmetrized. Black solid contours represent U/Ipeak at 0.05%, while red dashed contours represent U/Ipeak at −​​​​​​0.05%.
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: Stokes V mapping of J1407+2827 for the 19 beams near 1420 MHz. To compare with the simulated beam patterns, the mapping data have been mirror-symmetrized. Black solid contours represent V/Ipeak at 0.03%, while red dashed contours represent V/Ipeak at −0.03%.
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: Top: Stokes I mapping of J0854+2006 (2020), J0854+2006 (2021), and J1407+2827 (2022) for beams M01, M06, M017, and M18. The feature near the bottom of J0854+2006 is attributed to a nearby secondary source, J0854+1959. Contours (white lines) represent the fitting results, showcasing intensities at levels of 1%, 2%, 10%, 30%, 50%, 70%, and 90%, respectively. Bottom: Simulated total intensity beam patterns of M01, M06, M17, and M18. Contours are of the same intensity levels.
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: Simulated Stokes Q patterns of all 19 individual beams.
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: Simulated Stokes U patterns of all 19 individual beams.
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: Simulated Stokes V patterns of all 19 individual beams.
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: Spatial distribution of the time interval between SDSS and DESI observations. The purple curve represents the Galactic plane.
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: Distribution of the time intervals for celestial sources between the SDSS and DESI observations. The red dashed line represents the median value.
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: J-band image of TOI-5688 A and B taken with uTIRSPEC. A 10 × 10 pixel footprint from TESS Sector 40 is overlaid with the uTIRSPEC image, represented by the blue grid. The TESS aperture is highlighted in red, and both TOI-5688 A and B are marked. TESS observations of TOI-5688 A are contaminated by the presence of TOI-5688 B, making ground-based observations necessary to determine the true transit depth accurately.
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: Phase-folded transit light curves for TOI-5688 A b. Gray points represent the raw data. The model is shown in blue color for TESS and in red color for ground-based observations, along with the 1σ confidence intervals as translucent bands. The median statistical uncertainty is also shown at x = −0.05.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Green Chile Project. I. A New Catalog of Low-redshift Extended Emission-line Nebulae
Authors: Audrey F. Dijeau, Moire K. M. Prescott, Kelly N. Sanderson
Figure caption: Color–color plot of GC catalog objects. Our new cuts are represented by the pink solid lines. Overlaid are the color cuts from M. Schirmer et al. (2013; black dashed lines). The white circles are the 243 “raw” GC catalog objects, with the teal circles being the objects that remain after removing artifacts. The pink triangles are the GCs with existing SDSS spectra that have indications of AGN powering. The pink star is the GC with an existing SDSS spectrum that was previously identified as a GB in M. Schirmer et al. (2013). The purple squares and light pink plus signs are GCs with existing SDSS spectra that are not AGN-powered. The green stars are the original GBs from M. Schirmer et al. (2013).
Paper: The Green Chile Project. I. A New Catalog of Low-redshift Extended Emission-line Nebulae
Authors: Audrey F. Dijeau, Moire K. M. Prescott, Kelly N. Sanderson
Figure caption: Diagnostic diagram using emission-line measurements from SDSS/BOSS (A. S. Bolton et al. 2012). The blue stars are GBs (M. K. M. Prescott & K. N. Sanderson 2019). The empty green squares are the Green Peas (M. K. M. Prescott & K. N. Sanderson 2019). The dark magenta circles are the sample of Type 2 AGNs from S. Yuan et al. (2016). The pink triangles are GC objects. The GCs are labeled according to their GC Spec ID, indicated in Table 4. In the first two panels, the maximum star formation line, shown as the black line, is from L. J. Kewley et al. (2001). The dashed lines indicate ±0.1 dex. In the third panel, the black line shows 10% AGN contribution (M. Shirazi & J. Brinchmann 2012). The pink line is GC02, a source that lacked [N II], [S II], and Hα data, meaning it can only be represented one-dimensionally on these diagrams.