adsabs/AstroCLIMB huggingface dataset:
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Moment 0 maps (combination of the 12 m and 7 m arrays) of molecular lines toward G9.62+0.19. The white contours indicate the continuum emission, which is the same as in Figure 1. The black and white ellipses at the bottom-left corner indicate the angular resolution for the moment 0 maps of molecular lines and the continuum emission, respectively. Information of angular resolution, noise levels, and black contour levels are summarized in Table 6. The dashed squares in the panels of HC3N, SiO, and SO indicate the region in the other panels.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Moment 0 maps (combination of the 12 m and 7 m arrays) of molecular lines toward G10.47+0.03. The white contours indicate the continuum emission, which is the same as in Figure 1. The black and white ellipses at the bottom-left corner indicate the angular resolution for the moment 0 maps of molecular lines and the continuum emission, respectively. Information of angular resolution, noise levels, and black contour levels are summarized in Table 6.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Continuum images (λ = 2.75 mm, combination of the 12 m and 7 m arrays) toward five sources. The filled white ellipse indicates the angular resolution. Information about the noise level, contour level, and angular resolution for each panel is summarized in Table 4.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Moment 0 maps (combination of the 12 m and 7 m arrays) of molecular lines toward G19.88-0.53. The white contours indicate the continuum emission, which is the same as in Figure 1. The black and white ellipses at the bottom-left corner indicate the angular resolution for the moment 0 maps of molecular lines and the continuum emission, respectively. Information of angular resolution, noise levels, and black contour levels are summarized in Table 6. The dashed squares in the panels of CCH, HC3N, SiO, and SO indicate the region in the other panels.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Moment 0 maps (combination of the 12 m and 7 m arrays) of molecular lines toward G12.89+0.49. The white contours indicate the continuum emission, which is the same as in Figure 1. The black and white ellipses at the bottom-left corner indicate the angular resolution for the moment 0 maps of molecular lines and the continuum emission, respectively. Information of angular resolution, noise levels, and black contour levels are summarized in Table 6. The dashed squares in the panels of CCH and HC3N indicate the region in the other panels.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Moment 0 maps (combination of the 12 m and 7 m arrays) of molecular lines toward G16.57-0.05. The white contours indicate the continuum emission, which is the same as in Figure 1. The black and white ellipses at the bottom-left corner indicate the angular resolution for the moment 0 maps of molecular lines and the continuum emission, respectively. Information of angular resolution, noise levels, and black contour levels are summarized in Table 6. The dashed squares in the panels of CCH, HC3N, SiO, and SO indicate the region in the other panels.
Paper: Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules
Authors: Kotomi Taniguchi, Liton Majumdar, Paola Caselli, Shigehisa Takakuwa, Tien-Hao Hsieh, Masao Saito, Zhi-Yun Li, Kazuhito Dobashi, Tomomi Shimoikura, Fumitaka Nakamura, Jonathan C. Tan, Eric Herbst
Figure caption: Spectra of the CH3CN lines (J = 5 K −4 K , K = 0−4) at each core. The red curves show the best-fit results in the CASSIS software.
Paper: S-type Stars from LAMOST DR10: Classification of Intrinsic and Extrinsic Stars
Authors: Jing Chen, Yin-Bi Li, A-Li Luo, Xiao-Xiao Ma, Shuo Li
Figure caption: The equivalent widths of four important regions for intrinsic and extrinsic S-type stars. The dotted green and blue lines indicate the mean equivalent width for intrinsic and extrinsic S-type stars, respectively.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Systematic biases (solid black lines) and 1σ systematic uncertainties (gray shaded regions) in the recovery of T eff (top), ﹩\mathrm{log}g﹩ (middle), and [Fe/H] (bottom) as a function of resolution. All three labels are recovered with only very minimal differences (+1 K, −0.01 dex, and −0.03 dex) across the entire range of resolutions analyzed. Systematic uncertainties are similarly small.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: A portion of a synthetic spectrum generated wit the Payne (top) and its fractional flux uncertainty (bottom). The total model uncertainty is the quadrature sum of the three components displayed here: the median interpolation error (MIE) of the Payne (gray), NLTE effects (blue), and saturated lines (yellow). For visibility, the MIE has been inflated by a factor of 10 in this figure. The saturated line masked from this portion of the spectrum is the Hγ line at λ4341.7.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: The same as Figure 9 except for velocity-based atmospheric parameters v  r  (top), v macro (middle), and v micro (bottom). v  r  is recovered consistently at all resolutions with small systematic uncertainties (≲0.5 km s−1 for R ≳ 5000 and ∼1.5 km s−1 for R ∼ 2500). v macro exhibits distinct trends between the U09H observations (red squares) and the 147Hr and C316Hr observations (orange triangles and blue circles, respectively). The large systematic offsets seen at low resolution for the latter observations is attributed to incorrectly specified instrumental broadening. We recover v micro ≲ 0.5 km s−1 higher at lower resolutions consistent with its correlation with [Fe/H] and the small trend seen for [Fe/H] in Figure 9.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for iron-peak elements V (top), Cr (middle), and Mn (bottom). [V/H] and [Cr/H] are recovered consistently down to R ∼ 5000 with gradually increasing systematic uncertainties and a slight bias toward higher values at the lowest resolution. These systematic trends are driven by a combination of blending of imperfectly modeled lines in the blue and imperfectly modeled continuum regions in the red. Upper limits on [Mn/H] are recovered at all resolutions.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for C (top), N (middle), and O (bottom). We recover [C/H] consistently with small uncertainties at all resolutions. Resolution-dependent systematics are challenging to quantify for [N/H] and [O/H] due to the measurement of lower limits. For the U09H observations, the measurement of [N/H] appears consistent as a function of resolution. The measurement of [O/H] from these spectra is particularly challenging as most of the information comes indirectly from O’s impact on the atmospheric structure.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Marginalized posteriors for [Fe/H] (left) and [N/Fe] (right) for K431 observed in the C316Hr program at the degraded resolution of R ∼ 20,000. Posterior samples and the best-fit truncated normal distribution for the five individual exposures are plotted in the thin colored dashed histograms and solid curves, respectively. The stacked posterior recovered when combining the individual likelihoods is plotted as the thick black line. In the case of [N/Fe], the best-fit value is at the boundary of our priors (set by the extent of our training grid), necessitating the use of a truncated distribution.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for α elements Mg, Si, Ca, and Ti (from top to bottom). We find the recovery of [Mg/H], [Ca/H], and [Ti/H] to be consistent as a function of resolution down to R ∼ 2500. Larger uncertainties on [Mg/H] are due to the masking of NLTE-sensitive lines. [Si/H] displays a substantial bias with resolution and large systematic uncertainties as a result of its strong dependence on the stellar atmospheric structure.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for iron-peak elements Cu (top) and Zn (bottom). We find the recovery of [Cu/H] and [Zn/H] to be strongly resolution dependent with both large biases and uncertainties. These systematic effects are driven by the reliance on only a handful of lines that are influenced by the modeling of neighboring lines at lower resolutions.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for iron-peak elements Fe (top), Co (middle), and Ni (bottom). We find very small (≲0.03 dex) systematic effects for [Fe/H]. [Co/H] and [Ni/H] are also recovered consistently at all resolutions, though [Co/H] exhibits a substantial ∼0.3 dex systematic uncertainty at the lowest resolutions.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: The same as in Figure 7 but for three cases of host-galaxy-corrected spectra from the SDSS sample with diverse spectral properties to illustrate the fantasy multicomponent fittings: SDSS J010226.31-003904.5 (upper), SDSS J094620.86+334746.9 (middle), and SDSS SDSS J093641.05+101415.9 (bottom). All components used in the fitting model (broken power-law continuum and emission line features) are indicated with different colors (see the text for details).
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Multicomponent fitting with the fantasy code of the I Zw 1 observed spectrum (gray line) in the 4000–6800 Å wavelength region. The model (red line) consists of a broken power law (black dashed line), narrow lines (green solid line), broad (blue solid line) and intermediate (blue dashed line) components of the Balmer lines (Hα, Hβ, and Hδ) and He I lines (yellow line), intermediate components of [O III] (blue dashed line), the Fe II model (dark red line), and [Fe II] lines (light red line). The bottom panel shows a zoomed-in view of the observed (gray line), model (red line), and residual spectra (black line).
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Total Fe II emission in the pop A (full blue circles) and pop B (open red circles) subsamples with respect to the Hα (left) and Hβ (right) luminosities, in ergs per second. The Pearson correlation coefficient together with the corresponding p-value is indicated in each plot.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Balmer decrement Hα/Hβ vs. Hβ/Hγ (left) for the pop A (blue) and pop B (red) subsamples. The middle and right panels show Hα/Hβ and Hβ/Hγ vs. the ratio of the continuum luminosities at 5100 and 6200 Å. A significant anticorrelation is seen with the continuum ratio: for pop A objects r = −0.51 (p 0 ≪ 0.01) for Hα/Hβ and r = −0.40 (p 0 ≪ 0.01) for Hβ/Hγ, and for pop B objects r ∼ −0.39 (p 0 ≪ 0.01) for Hα/Hβ and r = −0.25 (p 0 ≪ 0.01) for Hβ/Hγ.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Left: SDSS sample plotted on the main-sequence diagram (FWHM(Hβ) vs. R Fe II ). Horizontal (FWHM(Hβ) = 4000 km s−1) and vertical (R Fe II  = 1) lines divide the pop B, pop A, and xA subsamples. The Eddington ratio (L/L Edd) is shown on the color bar. Right: Same diagram produced using the Hα FWHM and Fe II red (6100–6650 Å) emission. Pops A and B identified through the upper main sequence are marked with different symbols. Dashed and solid lines mark the position of FWHM(Hα) = 4000 km s−1 and FWHM(Hα) = 3500 km s−1, respectively.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Upper panels show the luminosity of Fe II in the three bands (Fe II blue (left), Fe II green (middle), and Fe II red (right)) as a function of the continuum luminosity L 5100 (given in ergs per second) for the pop A (full circles) and pop B (open circles) subsamples. The bottom panels shows only the subsample of xA objects. The Pearson correlation coefficient together with the corresponding p-value is indicated in each plot.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: An example of the AGN component (blue line) reconstructed after subtracting the contribution of the stellar component of the host galaxy (green line) from an observed spectrum (gray line) of SDSS J033013.26-053236.0. The host galaxy emission contributes on the level of 76% to the observed continuum flux around 6000 Å.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Balmer decrement Hα/Hβ (left) and Hβ/Hγ (right) for the pop A (blue) and pop B (red) subsamples vs. Eddington ratio (L/L Edd). The Pearson correlation coefficients point to no correlations: for the pop A objects r = 0.05 (p 0 = 0.3) for Hα/Hβ and r = −0.22 (p 0 < 0.01) for Hβ/Hγ, and for the pop B objects r ∼ −0.24 (p 0 < 0.01) for Hα/Hβ and r ∼ −0.16 (p 0 = 0.01) for Hβ/Hγ.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Luminosity (in ergs per second) of the broad Hα (left), Hβ (middle), and Hγ (right) lines as a function of the continuum luminosity λ L cnt at 5100 Å (upper panels) and for broad Hα vs. Hβ (left), Hα vs. Hγ (middle), and Hβ vs. Hγ (right) for the whole SDSS sample (bottom panels). The Pearson correlation coefficient together with corresponding p-value is indicated in each plot.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Total Fe II emission in the pop A and pop B subsamples (left), and for the xA subsample (right) with respect to the Eddington ratio L Edd/L bol.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Width of the broad Hβ plotted against the width of the broad Hα line (left) for the total SDSS sample, as well as the width of Fe II emission vs. Hα (middle) and Hβ (right) broad line width. Line widths are in kilometers per second. A linear best-fitting line is displayed in the Hβ vs. Hα plot, whereas in the two plots dashed lines denote the average values for the total sample.
Paper: Fantastic Fits with fantasy of Active Galactic Nuclei Spectra: Exploring the Fe II Emission near the Hα Line
Authors: Dragana Ilić, Nemanja Rakić, Luka Č. Popović
Figure caption: Correlations between the luminosity of Fe II in the three bands (Fe II blue (4340–4680 Å), Fe II green (5100–5600 Å), and Fe II red (6100–6650 Å)) for the pop A (blue circles) and pop B (red circles) subsamples (upper panels), and only for the population of xA objects (bottom panels). The Pearson correlation coefficient together with corresponding p-value is indicated in each plot.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for neutron-capture elements Sm, Eu, Gd, and Dy (from top to bottom). The recovery of [Gd/H] and [Dy/H] appears consistent, albeit with rapidly increasing uncertainties down to R ∼ 2500. We find that [Sm/H] is well recovered down to R ∼ 10,000, but exhibits increasing bias at lower resolutions. The measurement of [Gd/H], [Dy/H], and [Sm/H] are all characterized by fitting many very weak lines in crowded regions of the stellar spectrum. The presence of lower limits for [Eu/H] prevents robust quantification of the resolution-dependent systematic effects on its recovery. [Eu/H] also suffers from substantial NLTE effects and hyperfine splitting in their strong resonance lines.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Median correlations in the measurements of all 33 elemental abundances, v  r , v macro, and v microat R ∼ 10,000. Each panel depicts the correlation of a different pair of labels with the color of the panel indicating the strength and direction of the correlation. While most labels are not strongly correlated with one other, labels that contribute to a large number of pixels across the observed wavelength range like Fe, C, Mg, Si, and Ti exhibit modest correlations.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Top left: histogram of the median interpolation error of each model in the cross-validation set. The median error is consistently larger for higher-metallicity stars ([Fe/H] > −2; red) compared to lower-metallicity stars ([Fe/H] > −2; blue). Top right: cumulative percentage of pixels in each spectrum as a function of the median interpolation error. Approximately 80% of pixels have σ MIE < 0.001, and 95% of pixels have σ MIE < 0.006. Bottom: the median interpolation error across the cross-validation set as a function of wavelength. Errors are largest in the proximity of strong H lines and complicated molecular features.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for neutron-capture elements Er (top) and Th (bottom). The recoveries of [Er/H] and [Th/H] are all made difficult due to a paucity of absorption lines in the observed spectra. The recovery of [Er/H] exhibits a substantial bias toward larger values as the resolution is decreased. A negative bias is apparent for the few instances in which [Th/H] can be recovered below R ∼ 10,000.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for neutron-capture elements Sr, Y, Zr, and Ba (from top to bottom). We recover [Y/H] and [Zr/H] consistently down to R ∼ 5000 and with small positive and negative biases, respectively, at R ∼ 2500. We recover [Sr/H] with a slight positive bias at lower resolution. The presence of lower limits prevents the robust quantification of systematics for [Ba/H]. The measurements of both [Sr/H] and [Ba/H] suffer from substantial NLTE effects and hyperfine splitting in their strong resonance lines.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Fractional difference in the formal statistical uncertainty on [X/H] and the precision forecasted by the CRLB. Points and error bars represent the median and 16th and 84th percentiles across all individual exposure measurements performed in this study. For ∼85% of the elements considered here, the uncertainties are in general agreement. Large deviations from zero are found in instances of non-Gaussian posteriors (e.g., C, N, and O) and/or substantial model-data mismatches (e.g., Sr and Eu).
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Systematic biases (solid black lines) and uncertainties (gray shaded regions) in the recovery of elements at R ∼ 10,000 as a function of S/N. The median formal statistical uncertainties (blue shaded regions) are included for reference. Only elements that were found to have minimal resolution-dependent systematics in Section 4.1 are included. Most of these elements display S/N-dependent systematic effects that are small compared to the statistical uncertainties, though a few (C, Mg, Ca, and Dy) are biased at very low S/N.
Paper: Validating Stellar Abundance Measurements from Multiresolution Spectroscopy
Authors: Nathan R. Sandford, Daniel R. Weisz, Yuan-Sen Ting, 源森 丁
Figure caption: Same as Figure 9 except for neutron-capture elements La, Ce, Pr, and Nd (from top to bottom). We find a strong resolution dependence for the recovery of [Ce/H] and [Pr/H] as a result of blending in the feature-dense region around 4000 Å. The recovery of [La/H] appears similarly biased, though the presence of lower limits prevents robust quantification of the systematic effects. [Nd/H] is recovered consistently as a function of resolution with modest systematic uncertainties.