adsabs/AstroCLIMB huggingface dataset:
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: (a) Broadening functions of HPF spectra of the 21 M and K dwarf targets observed as part of the Gaia-ASOI exoplanet candidate list. The first six show systems that are compatible with being single lined, although, as highlighted in the text, Gaia-ASOI-16 could be a SB 2 due to the broad spectrum and line-width variations. The last 15 show systems that clearly exhibit double lines. If double lines are seen for a system, we pick one such observation where they are clearly seen, which we highlight in bold. The faint gray lines show the other epochs we obtained, showing that sometimes the targets are initially seen to be single lined and later split into two lines. In the cases where two double lines are seen, we additionally show best-fit Gaussians fit to the two peaks, where the blue peak shows the larger peak (larger total integrated area), while the red curve shows the secondary peak. (b) Similar to above, but showing the NEID CCFs. Gaia-ASOI-1 is the only single system, whereas the others clearly show double lines. In both (a) and (b) we first highlight the single-lined systems and then the SB 2 systems, and within those groups the systems are sorted by the presumed host-star mass. The host-star mass should be taken with caution for the SB 2 systems, as it assumes a single star.
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Eccentricities of substellar objects orbiting 0.1–0.7M⊙ stars. Only objects for which the statistical significance of the mass measurement is better than 3σ are shown. (a) Eccentricity as a function of companion mass. (b) Histograms of the orbital eccentricities for companion masses between 1 and 13MJ (blue) and between 13 and 80MJ (red). Gaia-4b and Gaia-5b are shown with green and orange stars, respectively. The stellar limit (~80MJ) and brown dwarf limit (13MJ) are highlighted with dotted and dashed lines, respectively. Circles represent true mass measurements while triangles are for companions for which only ﹩m\sin i﹩ is known. The eccentricity distributions of the low-mass and high-mass companions appear different; the low-mass sample includes more circular orbits. Planetary data were obtained from the NASA Exoplanet archive (R. L. Akeson et al. 2013), and brown dwarf data were obtained from Exoplanets.eu and A. T. Stevenson et al. (2023).
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Color–magnitude diagram of Gaia astrometric candidate planets and substellar objects. The 28 systems observed as part of this work are highlighted with stars or squares, while other systems from the literature are highlighted with the circles. Confirmed substellar companions are highlighted in green. Systems that are consistent with single stars but have yet to have a Gaia astrometric companion fully confirmed are highlighted in blue. Double-lined binary systems (SB 2) are highlighted in red. Systems that have an unknown designation are shown with white circles. The three Gaia-ASOI systems for which the Gaia astrometric solution was retracted are shown with black crosses. Gaia-4b and Gaia-5b are highlighted with the green star markers. For comparison, the Gaia Catalog of Nearby Stars (Gaia Collaboration et al. 2021) is shown with faint gray points in the background.
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Results from joint sampling of the Gaia two-body solution and RV of Gaia-4b. (a) Black data points are from HPF, blue diamond points are from NEID, and green squares are from FIES. The red curve is the best-fit joint Gaia+RV model, and the red shaded region is the 1σ credible interval. (b) Residuals. (c)−(d) Same as in (a)−(b) but as a function of orbital phase instead of time. (e) Comparison of the Thiele–Innes coefficients in the Gaia-only solution (black) and the joint Gaia+RV solution (red). (f) Z-scores of the Gaia+RV-sampled Thiele–Innes coefficients along with e, P, and tp. In all cases the Gaia and RV results are in agreement. (g) Astrometric orbit of the photocenter, after subtraction of parallax and proper motion. The black and blue curves show 1000 random draws based on the Gaia-only likelihood and the Gaia+RV likelihood, respectively. The + sign marks the center of mass, and the red square marks the periastron position. The dashed line is the line of nodes, and the arrow indicates the direction of the motion along the orbit. The RVs are available in digital form as data behind the figure and in Table 5.
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Masses of planets and brown dwarfs as a function of stellar host mass for stars with <0.7M⊙ and orbital periods <104 days. (a) Companion mass as a function of host-star mass. (b) Histogram of the points in panel (a). (c) Mass ratio as a function of host-star mass. The stellar limit (~80MJ) and brown dwarf limit (13MJ) are highlighted with the dotted and dashed lines, respectively. Gaia-4b and Gaia-5b are highlighted with the green and orange stars, respectively. Companions with minimum mass measurements (﹩m\sin i﹩) are shown with triangles, while true mass measurements (m) are shown with the circles. Only companions with better than 3σ mass measurements are shown. We highlight the lack of 1 to ~10MJ planets around ≤0.3M⊙ with the blue “Jupiter desert” region. Planetary data are obtained from the NASA Exoplanet archive (R. L. Akeson et al. 2013), and brown dwarf data are obtained from Exoplanets.eu and A. T. Stevenson et al. (2023).
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Astrometry-predicted RV orbits for (a) Gaia-4b and (b) Gaia-5b compared to the RV observations from HPF (black points), NEID (blue points), and FIES (green points). The red curve shows the expected best model as predicted from the Gaia solution (no fit with the RVs has been performed), and the red shaded region shows the 1σ region from the expected Gaia orbit. For Gaia-5b, we show the astrometry-predicted RV solution with ω + 180°, due to the 180° degeneracy in ω in the Gaia two-body solution. The RVs agree with the expected RV orbit from the Gaia two-body solutions.
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Stellar rotation period for Gaia-4b. (a) ASAS-SN photometry as a function of time. (b) Generalized Lomb–Scargle periodogram of the photometry in (a) showing a clear peak at 13.3 days (red vertical line) with a false-alarm probability (FAP, gray dashed line)  ≪ 1%. The 1 day alias of the 13.3 day period is shown with the blue vertical line. We adopt a stellar rotation period of 13.3  ±  1.3 days.
Paper: Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
Authors: Gudmundur Stefánsson, Suvrath Mahadevan, Joshua N. Winn, Marcus L. Marcussen, Shubham Kanodia, Simon Albrecht, Evan Fitzmaurice, Onė Mikulskytė, Caleb I. Cañas, Juan I. Espinoza-Retamal, Yiri Zwart, Daniel M. Krolikowski, Andrew Hotnisky, Paul Robertson, Jaime A. Alvarado-Montes, Chad F. Bender, Cullen H. Blake, J. R. Callingham, William D. Cochran, Megan Delamer, Scott A. Diddams, Jiayin Dong, Rachel B. Fernandes, Mark R. Giovinazzi, Samuel Halverson, Jessica Libby-Roberts, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Jayadev Rajagopal, Varghese Reji, Arpita Roy, Christian Schwab, Jason T. Wright
Figure caption: Same as Figure 3, but for Gaia-5b. The RVs are available as data behind the figure and in Table 6.
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: The ratio of the average Lacc,line with L* for each star for which Lacc,line had been measured. The ratio is plotted in a logarithmic scale against Teff. Class II YSOs are plotted in black, and the two class III YSOs are plotted in green. The red and orange dashed lines mark the approximate boundary below which chromospheric emission becomes an important contributor to Lacc, according to C. F. Manara et al. (2013b) and C. F. Manara et al. (2017a). The blue dashed line marks the same but according to R. A. B. Claes et al. (2024), with the Teff scale converted from G. J. Herczeg & L. A. Hillenbrand (2014) to the one used in this work in Section 4.1. Objects 4 and 13, having only an approximate Lacc,line, are represented with open circles.
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: Plot of log(Macc) vs. log(M*) for the class II targets of our current sample, compared to the results for class II YSOs from Lupus (J. M. Alcalá et al. 2017), Chamaeleon I (C. F. Manara et al. 2016), and NGC1333 (E. Fiorellino et al. 2021). These three sets are plotted in magenta, blue, and orange, respectively, with upper limits represented by triangles. The values from this work are plotted in black and gray, with different shapes for different regions: circles (NGC 1333), stars (NGC 7000), squares (IC 5146), a diamond (Serpens), a plus sign (Orion), and an X-symbol (Perseus). Object 4 in NGC 7000, having only an approximate Macc, is represented with an unfilled star.
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: The median model fit for Object 1 and the parameter posteriors below (the median parameters marked with a vertical gray dotted line).
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: Plot of the continuum-derived log(Lacc) vs. log(L*) for the class II targets of our sample, compared to the results for class II YSOs from Lupus (J. M. Alcalá et al. 2017), Chamaeleon I (C. F. Manara et al. 2016), and NGC 1333 (E. Fiorellino et al. 2021). These three sets are plotted in magenta, blue, and orange, respectively, with upper limits represented by triangles. The values from this work are plotted in black and gray, with different shapes for different regions: circles (NGC 1333), stars (NGC 7000), squares (IC 5146), a diamond (Serpens), a plus sign (Orion), and an X-symbol (Perseus). Object 4, having only an approximate Lacc, is represented with an unfilled star.
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: The overlaid posteriors for log(Lacc) and log(L*) vs. AV, for every object in our sample in which log(Lacc) is not an upper limit or is approximated. A strong correlation can be seen between AV and log(Lacc) in particular.
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: Plot of log(Macc) vs. the spectral index α used for YSO classification in Section 3. Class II YSOs are plotted in black, and Class III YSOs are plotted in green. Upper limits in Macc are denoted by downward triangles. Objects 4 and 13, having only an approximate Macc, are represented with open circles. The blue line is the dividing line between Class II and Class III in T. P. Greene et al. (1994).
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: The median model fit for Object 2 and the parameter posteriors with the same plotting convention as Figure 21.
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: The corner plot for Object 1, for model parameters and the log(L*) and log(Lacc) posteriors.
Paper: A Bayesian Approach to Inferring Accretion Signatures in Young Stellar Objects: A Case Study with VIRUS 
Authors: Lauren Halstead Willett, Joe P. Ninan, Suvrath Mahadevan, Gregory R. Zeimann, Steven Janowiecki, Gary J. Hill
Figure caption: The corner plot for Object 2, for model parameters and the log(L*) and log(Lacc) posteriors.
Paper: JWST 1.5 μm and 4.8 μm Photometry of Y Dwarfs
Authors: Loïc Albert, Sandy K. Leggett, Per Calissendorff, Thomas Vandal, J. Davy Kirkpatrick, Daniella C. Bardalez Gagliuffi, Matthew De Furio, Michael Meyer, Charles A. Beichman, Adam J. Burgasser, Michael C. Cushing, Jacqueline Kelly Faherty, Clémence Fontanive, Christopher R. Gelino, John E. Gizis, Alexandra Z. Greenbaum, Frantz Martinache, Mamadou N'Diaye, Benjamin J. S. Pope, Thomas L. Roellig, Johannes Sahlmann, Anand Sivaramakrishnan, Marie Ygouf
Figure caption: F480M vs. F150W – F480M color–magnitude diagrams. Black circles represent new measurements presented here. Colored dots are synthesized colors from S. A. Beiler et al. (2024) where the symbol color indicates Teff, determined by Beiler et al. from luminosity measurements. Colored rings similarly indicate Teff; the symbol color for a given Teff range is indicated along the right axis of the top-left panel. The warmest and coldest objects in our sample, the WISE-0336 binary system, and outliers, are identified in the top-left panel. The other panels compare the data to various model sequences; surface gravity and metallicity properties are indicated by line type as shown in the legend in the top-right panel. Sequences in the top-right panel are from disequilibrium-chemistry and adiabat-adjusted ATMO2020++ models (S. K. Leggett et al. 2021; A. M. Meisner et al. 2023). The middle panels show Sonora sequences, equilibrium-chemistry Bobcat on the left (M. S. Marley et al. 2021) and disequilibrium-chemistry Elf Owl on the right (S. Mukherjee et al. 2024). The bottom panels show disequilibrium-chemistry models from B. Lacy & A. Burrows (2023) with and without water clouds. Model Teff values are indicated along the right axes and plus symbols along the model sequences indicate colors at those Teff. For the Elf Owl panel the outer axis Teff values refer to the metal-poor sequence and the inner values to the solar-metallicity sequences; for the other models the M480M values are more similar across the metallicity range.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Relative positions of source 0723−008 at optical and radio wavelengths with a MOJAVE radio image at 15 GHz in the background. The MOJAVE image selected is from 2023 July 8 and is the closest in time to session vr2302 (carried out on 2023 May 31), the only quad-band session where source 0723−008 was observed.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Distribution of normalized arc lengths between the quad-band and S/X positions. The blue bars correspond to the normalized arc lengths based on the original uncertainties of the quad-band positions, whereas the red bars correspond to those derived with inflated uncertainties. The normalized arc lengths exceeding 5.0 are counted in the last bin. The Rayleigh distribution is shown as the gray curve.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Sky distribution of 377 radio sources in the quad-band position catalog. The color coding depicts the length of the semimajor axis of the position error ellipse in four predefined ranges, as printed in the bottom right-hand corner.
Paper: New Stellar Parameters, Metallicities, and Elemental Abundance Ratios for 311 Metal-poor Stars
Authors: Sanil Mittal, Ian U. Roederer
Figure caption: Comparison of Teff values found in this study and I. U. Roederer et al. (2014). The new values are 310 ± 164 K warmer on average. The dashed line indicates a 1:1 ratio. Only statistical uncertainties are shown. The size of the error bars are comparable to the size of the markers, making it difficult to see them.
Paper: Variations of Absolute Source Positions Determined from Quad-band VLBI Observations
Authors: Ming Hui Xu, Patrick Charlot
Figure caption: Source position offsets between quad-band and S/X band as a function of decl. The error bars are calculated by adding in quadrature the uncertainties of the S/X positions in the ICRF3 to the inflated uncertainties of the quad-band positions. The green triangles highlight the position offsets that are significant at the 3σ level.
Paper: New Stellar Parameters, Metallicities, and Elemental Abundance Ratios for 311 Metal-poor Stars
Authors: Sanil Mittal, Ian U. Roederer
Figure caption: Comparison of log g values found in this study and I. U. Roederer et al. (2014). The new values are 0.64 ± 0.35 higher on average. The dashed line indicates a 1:1 ratio. Stars that lie along the 1:1 line are stars for which precise parallax values were available to I. U. Roederer et al. (2014).
Paper: New Stellar Parameters, Metallicities, and Elemental Abundance Ratios for 311 Metal-poor Stars
Authors: Sanil Mittal, Ian U. Roederer
Figure caption: Comparison of microturbulence velocity vt values found in this study and I. U. Roederer et al. (2014). The new values are 0.06 ± 0.19 km s−1 higher on average. The dashed line indicates a 1:1 ratio.
Paper: New Stellar Parameters, Metallicities, and Elemental Abundance Ratios for 311 Metal-poor Stars
Authors: Sanil Mittal, Ian U. Roederer
Figure caption: Comparison of model metallicity [M/H] values found in this study and I. U. Roederer et al. (2014). The new values are on average 0.27 ± 0.14 dex higher. The dashed line indicates a 1:1 ratio.