adsabs/AstroCLIMB huggingface dataset:
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Effective time derived from the spectroscopic TSNR values (T spec; see Equation (22)) as a function of the effective time T r from Equation (23).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Comparison of the g − r colors from the targeting catalog with the colors inferred from the stellar spectrum fit. Each dot is a standard star from a typical 900 s exposure.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Example of a CTE issue for the petal (3) for one night identified by the QA. From top left to bottom right: median counts over the 21 rows just above and/or below the CCD amplifier boundary for a flat field exposure, redshift vs. the fiber number for petal (3) (sky-subtracted) sky fibers for all dark tiles from that night, an ELG spectrum drawn from one of the impacted fibers. See text for more details.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: TOIs by stellar effective temperature and planet candidate radius. The temperature and planet radius distributions of the TOIs show a marked drop toward late spectral types (>M4–M6) and for small planets (R  p  < 2 R ⊕). The green shaded region represents the sensitivity of our EDEN survey, which is complementary to that of TESS.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: The average sensitivity (top) and full detection probability including the geometric transit likelihood (bottom) of the EDEN survey for planets with periods between 0.5 and 10 days and sizes between 0.6 and 3.5 Earth radii. For ultrashort-period planets (<1 day), we reach 50% sensitivity for planets with radii of 1.5 R ⊕ or larger. Due to the low geometric transit probabilities, the overall completeness is much lower and drops sharply with orbital period. The inner edge of the habitable zone is defined using the Kopparapu et al. (2013) model based on temperature and insolation (assuming a stellar effective temperature of 2600 K and a planetary albedo of 0.3).
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: The first look at the nondetrended light curves from a simple reference star calibration of each potential transit event, before full detrending is done. The transit-like features are marked with green lines and the name of the Project EDEN member who analyzed the quick look data.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: The upper limits on the occurrence rates from our analysis that follows the procedure from Sagear et al. (2020), assuming P null = 0.05. We find similar occurrence rates when adjusting for bin size and type (log-linear vs. log–log in orbital period and planet radius) for, e.g., mini-Neptune planets with orbital periods just greater than 1 day.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: A detrended light curve with an injected transit from the Kuiper 61″ telescope on 2021 November 7 UT. The transit is deep enough that the detrending raises the baseline pre- and post-transit slightly compared to the rest of the light curve, but this does not affect our ability to recover the injected planet because it is such a strong signal (S/N ∼ 6).
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: The three light curves (both full and 10 minutes binned data) with errorbars for EIC 9 where we identified transit-like features (noted by the black vertical lines in each panel). Top: light curve from LOT on 2020 November 18 (UT); the transit event originally identified (see Figure 5) is centered at 7.8 hr (2459172.33 JD). Middle: light curve from Kuiper on 2020 November 18 (UT) with the transit event centered at 6.8 hr (2459172.91 JD). Bottom: light curve from VATT on 2020 December 22 (UT); the transit event is centered at 6.1 hr (2459206.91 JD).
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: Additionally detrended light curves for EIC 9. Top: follow-up light curve from Calar Alto in January 2021 with no transit feature near the expected mid-transit time from the TESS period (red dashed line). Middle: LOT light curve from 2020 November with the expected mid-transit time from TESS marked. No transit-like signal is visible. Bottom: Kuiper telescope light curve from 2020 November, with the expected mid-transit time from a 2.886 day period. Here, a transit-like feature is visible.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: Sensitivity maps for the targets found to be binary stars, EIC 10 and 14.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: Sensitivity maps for EIC 1, 2, 4, 5, 6, 7, 8, and 9.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: Sensitivity maps for EIC 20, 21, 22, and 23.
Paper: EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates of Planets around Late-M Dwarfs within 15 pc
Authors: Jeremy Dietrich, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman, Benjamin V. Rackham, Nicolas Kurtovic, Karan Molaverdikhani, Paul Gabor, Thomas Henning, Wen-Ping Chen, Luigi Mancini, Alex Bixel, Aidan Gibbs, Richard P. Boyle, Samantha Brown-Sevilla, Remo Burn, Timmy N. Delage, Lizxandra Flores-Rivera, Riccardo Franceschi, Gabriele Pichierri, Sofia Savvidou, Jonas Syed, Ivan Bruni, Wing-Huen Ip, Chow-Choong Ngeow, An-Li Tsai, Chia-Lung Lin, Wei-Jie Hou, Hsiang-Yao Hsiao, Chi-Sheng Lin, Hung-Chin Lin, Ritvik Basant
Figure caption: Sensitivity maps for EIC 11, 12, 13, 15, 16, 17, 18, and 19.
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Steps to separate the Hα spectra in time series of LTT 1445B and C from Data Set 1. Panel (a): stacked spectrum of raw images from Data Set 1. Panel (b): zoomed in to the spectral region around the Hα line. Hα emission is visible by eye in stars B and C, but not in A. Panel (c): pixels are summed in the spatial direction, as indicated by the dashed lines in Panel (b), and plotted along the dispersion axis. Hα is present in emission for both LTT 1445 B and C. Panel (d): we sum the counts in a box of pixels around the Hα lines in both B and C as indicated by the dashed lines. We do this for each exposure across the time span where we see the flare in Data Set 1. Panel (e): counts as a function of time for B and C. It is clear that the flare in Data Set 1 occurring around the 95th minute after the start of the time series originates from LTT 1445C.
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Transmission spectra from Data Sets 1–4. The spectroscopic data are binned to 20 nm and the individual transmission spectra are offset for clarity in the x-axis. Bars in the y-axis represent 68% confidence intervals, with black bars representing the inverse-variance weighted mean value of ﹩{({R}_{{\rm{p}}}/{R}_{{\rm{s}}})}^{2}﹩ in each bin; black bars along the x-axis illustrate the extent of each bin in wavelength.
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Normalized Hα (655–658 nm) light curves from LTT 1445BC in each of the four data sets analyzed in this work. Gray points in the background are the integrated broadband flux in each data set. The data are not flux calibrated so the light curves are presented as normalized flux. We multiply the broadband flux variability (gray points) by a factor of 10 so as to easily compare to the variability in the Hα-only light curves. The inset shows a broadband flare identified in Data Set 1.
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Observed transmission spectrum of LTT 1445Ab from four data sets combined (black points the same as in Figure 5) compared to model transmission spectra derived from 1× solar composition atmospheres from 0.01 to 10 bars of surface pressure. The σ values in the legend are the confidence to which we can rule out the corresponding model transmission spectrum. We confidently rule out (to 3.2σ) a 1× solar composition atmosphere with 10 bars of surface pressure, and (to 3.1σ) the same atmosphere with with 1 bar of surface pressure.
Paper: Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab
Authors: Hannah Diamond-Lowe, João M. Mendonça, David Charbonneau, Lars A. Buchhave
Figure caption: Left: spectroscopic light curves with the GP noise component removed for each of the 4 data sets. The transit model (GP mean function) is plotted in gray for each data set. Light curves are offset for clarity. Right: residuals compared to the best-fit transit model for each of the four data sets along with the combined rms. The individual transit depths and uncertainties are provided in Table 4 and shown in Figure 5.
Paper: Equalizing the Pixel Response of the Imaging Photoelectric Polarimeter Onboard the IXPE Mission
Authors: John Rankin, Fabio Muleri, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Matteo Bachetti, Luca Baldini, Enrico Costa, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Martin C. Weisskopf, Fei Xie
Figure caption: Example of a photoelectric track on the GPD. The part in darker color, with the greatest charge density (the Bragg peak), is the one formed last. The part with less charge is the one containing the real polarimetric information. the reconstruction algorithm used to determine polarization (Manfreda 2020) identifies the Bragg peak first (left side of the figure) and then reconstructs the original direction (right side of the figure).
Paper: Equalizing the Pixel Response of the Imaging Photoelectric Polarimeter Onboard the IXPE Mission
Authors: John Rankin, Fabio Muleri, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Matteo Bachetti, Luca Baldini, Enrico Costa, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Martin C. Weisskopf, Fei Xie
Figure caption: Schematic of the GPD. See the text for details. Image credit: Weisskopf et al. (2016).
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Impact of different ﹩{\nu }_{t}\mbox{--}\mathrm{log}g﹩ relations. Left column: ﹩\mathrm{log}g﹩ vs. ν  t  for each sample of stars. The thin red lines at the bottom indicate the ﹩\mathrm{log}g﹩ of Ret II stars. The best quadratic fit is plotted as a thick red line. The gray points show stars from all other rows for context. Left-middle column: [Ba/H] vs. T eff. Right-middle column: [Ba/H] vs. [Fe/H]. Right column: [Ba/H] vs. S/N. Stars with S/N < 25 display substantially larger [Ba/H] scatter, likely due to residuals from sky subtraction. Overall, the first three rows (B05, C13, J15) have similar trends, showing an upturn in ν  t  at low ﹩\mathrm{log}g﹩ but a very noticeable trend in [Ba/H] vs. T eff. The last three rows have smaller ν  t  and little trend in [Ba/H] vs. T eff (excluding stars with S/N < 25).
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Comparison of [Ba/H] vs. T eff slopes for different microturbulence relations. In contrast to Figure 9, here we only include the high S/N clear member stars. The left and right panels show the NLTE and LTE [Ba/H] abundances, respectively. The red circles and blue squares indicate [Ba/H] derived using the R14g and B05                          ﹩{\nu }_{t}\mbox{--}\mathrm{log}g﹩ relations, respectively. The red and blue solid lines indicate a fit to all stars using the R14g and B05 relations, respectively, while the dashed lines indicate the fit removing the coolest star (ID 1). It is clear that the trend with T eff is flatter using the R14g relation, regardless of whether the coolest star is included. For the NLTE panel, the slopes of the lines (in units of dex per 100 K) are 0.03 and 0.08 for R14g and B05, respectively, or 0.01 and 0.05 when removing the cold star for R14g and B05, respectively.
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Differences between NLTE (MULTI/MARCS) and LTE (MOOG/ATLAS) abundances for stars with S/N > 25. Left: differences as a function of [Ba/H] (LTE). Right: differences as a function of T eff. The NLTE correction for saturated lines clusters closely around Δ[Ba/H] = −0.27 ± 0.04 (the outlier is the candidate member Star 14 with a relatively low [Ba/H] abundance).
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Exploration of different best-fit models by permuting the data sample (top-right panel), radiative transfer (bottom-left panel), and ﹩\mathrm{log}g\mbox{--}{\nu }_{t}﹩ relation (bottom-right panel).
Paper: Metal Mixing in the r-process Enhanced Ultrafaint Dwarf Galaxy Reticulum II 
Authors: Alexander P. Ji, Joshua D. Simon, Ian U. Roederer, Ekaterina Magg, Anna Frebel, Christian I. Johnson, Ralf S. Klessen, Mattis Magg, Gabriele Cescutti, Mario Mateo, Maria Bergemann, John I. Bailey
Figure caption: Abundance gradients. The x-axis on all plots is the elliptical radius, in units of the elliptical half-light radius. The symbols are as in Figure 5, with large red points indicating high-S/N stars with confident membership. There are no significant abundance gradients.