adsabs/AstroCLIMB huggingface dataset:
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: The combined V light curves of the longer-period objects (P ∼ 60–160 days), based on VUO-new (blue squares) and ASAS-SN (red circles) data, and normalized as described in the text. These are fitted by the periods, amplitudes, and phases recorded in Table 4. The data uncertainties are small, ±0.005–0.010 mag, except for IRAS 04296+3429 (±0.015 mag).
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: The frequency spectrum of the normalized V light curve of each of the objects. The period, in days, is listed in parentheses. For the two shorter-period objects, IRAS 07134+1005 and 19500–1709, we have also the frequency spectra of the larger-amplitude ASAS-SN g light curves. These are shown in the bottom row.
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: Plot showing the relationship between the maximum brightness change in a season (ΔV) and the effective temperature (T eff) of the stars. The values are much larger at the cooler temperatures and then decrease rapidly by T eff = 6500–7000 K. The stars from the present study are shown as filled circles, and those from other studies as open circles, as listed in Table 5. AFGL 2688 is not included because the measured variation in starlight is compromised by the large scattering area of the lobe. The dotted–dashed line is a free-hand representation of the trend in the data. Estimated average error bars of ±0.02 mag and ±250 K are shown.
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: The ASAS-SN g light curves of the shorter-period objects (P ∼ 30–40 days), normalized as described in the text, and fitted by the periods, amplitudes, and phases recorded in Table 4. The data uncertainties are small, <0.005 mag.
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: Plot showing the relationship between the pulsation periods and the effective temperatures of the stars. A clear inverse, linear relationship is found. The stars from this present study are shown as filled circles, those from other studies as open circles, and the one with a less-certain period shown with a smaller symbol, as listed in Table 5. The solid line in the bottom panel is a least-squares fit to the data between 5000 and 8000 K. Conservative average error bars of ±3 days and ±250 K are shown.
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: The ASAS-SN V light curves (red) and g light curves (blue), with the latter offset to the level of the V light curve for the interval of overlap. The amount of the offset in units of magnitudes is listed in parentheses.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The distribution of T  e [O III] in M33 measured by CHAOS and recalculated from the literature studies. Left Panel: A violin plot of the T  e [O III] measured from the different studies. The minimum, maximum, and number density of T  e [O III] are plotted as the base, peak, and width of each violin, respectively. Some of the violin profiles are affected by the relatively few recalculated T  e [O III] (e.g., C06 and T16). Right Panel: The average T  e [O III] and standard deviation measured from the distribution of T  e [O III] in each sample.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: A portion of the MODS 2D spectrum of M33+29+261 focused on Hγ, Hg I λ4358, [O III]λ4363, He I λ4388, and He I λ4471. Top Panel: The 2D spectrum before sky subtraction. The location of [O III]λ4363 is highlighted in the cyan box, and the line can be seen on the red edge of the Hg I λ4358 emission. With lower spectral resolution, [O III]λ4363 may be entirely blended with Hg I λ4358. The location of He I λ4388 is highlighted with the dashed magenta box. Bottom Panel: The 2D spectrum after sky subtraction. Hg I λ4358 is cleanly subtracted and the [O III]λ4363 emission is present within the cyan box. The 2D profile of [O III]λ4363 is comparable to the He I λ4388 feature, the latter of which is not susceptible to Hg I contamination.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The spectrum of M33−35−385 near Hγ. The lines [Fe II]λ4288, [Fe II]λ4360, and [O III]λ4363 can be made out in this wavelength range. Top Panel: A fit to the three emission lines while using the [O III] strong lines to constrain the Gaussian FWHM of [O III]λ4363 and the same FWHM for each [Fe II] line. Each line fit is provided as a colored Gaussian, while the linear continuum is plotted as an orange line. [Fe II]λ4360 and [O III]λ4363 can be deblended, and this produces a nondetection of [O III]λ4363. Bottom Panel: A fit to [Fe II]λ4288 and a line at 4361.5 Å, to simulate a single Gaussian fit to [O III]λ4363. The Gaussian for [O III]λ4363 is clearly too intense and too broad relative to the Gaussian with FWHM set by the strong lines, but the intensity is large enough to produce an erroneous line detection.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The oxygen abundance gradient in M33 as measured from CHAOS (65 regions, purple), T16 (six regions, orange), A22 (13 regions, green), and Esteban et al. (2009) (two regions, cyan). The best-fit gradient (dashed purple line) and intrinsic dispersion in O/H (shaded purple area) are provided in the legend. The point representation is the same as Figure 4.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: A cartoon image indicating the stretching of molecular gas as it travels along x 1 orbits, from apocenter to pericenter. The red circles represent the initial parcels of gas located at apocenter, and the red ellipses represent their elongated counterparts once they reach pericenter. The blue dotted lines indicate various x 1 orbits, and the black dotted lines indicate x 2 orbits. The shaded gray regions indicate possible dust lane placements. The black arrows show the direction of gas flow. The x 1 and x 2 orbits, as well as the factor by which the gas is stretched, were calculated using the same gravitational potential as used in Sormani et al. (2018; their orbits are shown in the top left panel of their Figure 8).
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Spectra for 12CO, 13CO, and C18O taken from four different regions and averaged over a circular aperture with a diameter that is three times larger than the semimajor axis of the beam. Regions 1 and 2 are pulled from two different locations along filament 1, whereas regions 3 and 4 are located along filament 2. The spectra for 13CO and C18O are scaled by factors of 2 and 8 and offset by 15 K and 30 K, respectively, so that they can be seen clearly. Spectral peaks are labeled with their corresponding velocity components identified in the p–v diagrams (Figures 8 and 9).
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: The full-resolution velocity channel maps for the spectral line C18O, with channel widths of ∼0.3 km s−1. The channel maps on the top row span the velocity range of −222.0 to −224.0 km s−1. The channel maps on the bottom row span the velocity range of −202.0 km s−1 to −204.0 km s−1. In each figure, the top—orange—contour indicates the region that we define for filament 1, while the bottom—blue—contour indicates the filament 2 region. The beam is indicated in the lower right corner of each channel map.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption:  l–v diagram of the 12CO (J = 3 − 2) emission (CHIMPS2; Eden et al. 2020) toward the Sgr E region, integrated over the range ﹩\left|b\right|﹩ < 0.°175. The data have a spatial resolution of 15″ and a velocity resolution of 1 km s−1. The black rectangle represents the boundary of the zoomed-in region shown at the bottom of the figure. The zoomed-in region spans the velocities −190 km s−1 to −230 km s−1. The red contours indicate the emission from the Sgr E 13CO data cube in the same l–v region at a temperature threshold of 0.0075 K.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Ratio maps for 12C16O/13C16O (top), 12C16O/12C18O (middle), and 13C16O/C18O (bottom). These ratio maps were calculated from the moment 0 maps seen in Figure 5, with some additional masking (see Section 3.3). The circles outlined in cyan indicate the regions that the spectra were averaged over. In the top image, the regions are labeled with the numbers assigned to the spectra in Figure 11.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: The full-resolution velocity channel maps for the spectral line 12CO, with channel widths of ∼0.3 km s−1. The channel maps on the top row span the velocity range of −222.0 km s−1 to −224.0 km s−1. The channel maps on the bottom row span the velocity range of −202.0 km s−1 to −204.0 km s−1. In each figure, the top—orange—contour indicates the region that we define for filament 1, while the bottom—blue—contour indicates the filament 2 region. The beam is indicated in the lower right corner of each channel map.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Continuum emission (3 mm) located toward our pointing of the Sgr E region. The top—orange—contour indicates the filament 1 region, while the bottom—blue—contour indicates the filament 2 region. The beam is indicated in the lower right corner of the figure.
Paper: Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
Authors: Wuming Yang
Figure caption: Top panels: relative sound-speed and density differences, in the sense (Sun-Model)/Model, between the Sun and models. The solar sound speed and density are given in Basu et al. (2009). Bottom panels: distributions of observed and predicted ratios r 02 and r 13 as a function of frequency. The circles and triangles show the ratios calculated from the frequencies observed by GOLF & VIRGO (García et al. 2011) and BiSON (Chaplin et al. 1999), respectively.
Paper: Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
Authors: Wuming Yang
Figure caption: Left panel: comparison of the Rosseland mean opacities of different models relative to that of Aopal12r. Right panel: distributions of the Rosseland mean opacities of the models as a function of radius.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Upper panels: comparison between the stellar E(B − V)UV with respect to the gas E(B − V), color coded as a function of ﹩\mathrm{log}(\mathrm{SFR})﹩ (on the left) and ﹩\mathrm{log}(\mathrm{sSFR})﹩ (on the right) within the COS aperture. The dashed black line represents the 1:1 relation, while the dotted line is the C97 empirical relation between the stellar and gas E(B − V) (i.e., E(B − V)UV = (0.44 ± 0.03) × E(B − V)). The uncertainties on the displayed quantities are shown in both axes. Lower panels: Δ(E(B − V)) defined as E(B − V) − E(B − V)UV. Δ(E(B − V)) increases linearly with E(B − V), and the linear best fit is indicated by the red solid lines, reported on the upper right, while the dashed and dotted lines represent the 1σ and 2.6σ around the best fit. The red horizontal dotted line represents the median Δ(E(B − V)) while the shaded red region shows the 68% intrinsic scatter of the distribution. Δ(E(B − V)) increases at increasing ﹩\mathrm{log}(\mathrm{SFR})﹩ and decreasing ﹩\mathrm{log}(\mathrm{sSFR})﹩. Overall, E(B − V) ∼ E(B − V)UV at ﹩\mathrm{log}({SFR}/[﹩                      M ⊙ yr−1]) ≲ −1.5 and ﹩\mathrm{log}({sSFR}/{{yr}}^{-1})\gtrsim -8﹩, whereas at higher SFRs and lower sSFRs the stellar vs. gas E(B − V) relation follows the C97 relation.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: log(U) estimated for low- (purple squares; S3S2 line ratio), intermediate- (green diamonds; O3O2 line ratio), and high-ionization regions (orange circles; Ar4Ar3 line ratio) as a function of C IV λλ1548,51/C III] λλ1907,09, log(EW(C IV λ λ 1548,51)), C III] λλ1907,09/O III] λ1666, and log(EW(Hα)). The uncertainties on the displayed quantities are shown in both axes. The red solid lines represent the best fit that we calculated between the observables shown and the three log(U) values, while the dashed and dotted lines show the 1σ and 2.6σ scatter around the relation. The best-fit equations as well as the intrinsic scatter are reported in the legend in each panel. The dashed–dotted purple line in the bottom figure, left panel, is the correlation found by Mingozzi et al. (2020) between log(U) and log(EW(Hα)). This figure shows the most promising UV tracers of log(U).
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Top panel: 12+log(O/H) as a function of the O III] λ1666/He II λ1640, C III]/O III] λ1666, C III]/He II λ1640, and C IV/C III] line ratios (upper panels), and EW(He II λ1640), EW(O III] λ1666), EW(C III]), and EW(C IV) (lower panels), color coded as a function of the ionization parameter log(U) derived from O3O2. The uncertainties on the displayed quantities are shown in both axes. All the quantities are in logarithm, and the Pearson factor and p value are shown in each panel. Overall the most promising relations are between C III]/[O III] λ1666, EW(O III] λ1666) < 4 Å and EW(C III]) with 12+log(O/H), but there is scatter in the plots, partly due to a degeneracy with the ionization parameter, as it can be appreciated from the color coding. Bottom panel: same for log(U), color coding as a function of 12+log(O/H) from Paper I.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Gas-phase metallicity, 12+log(O/H), as a function of C III]/O III] λ1666 (left panel) and EW(C III]) (right panel), color coded as a function of log(U). The uncertainties on the displayed quantities are shown in both axes. Our best-fit linear relations are shown by the solid red lines, while the dashed and dotted black lines represent the 1σ and 2.6σ around the best fit. The scatter in both panels can be partly explained by a secondary dependence on the ionization parameter. In the right panel we also include values found for star-forming galaxies studied in recent works (Rigby et al. 2015; Berg et al. 2016; Senchyna et al. 2017, 2019; Berg et al. 2019a; Schaerer et al. 2022), in which 12+log(O/H) was computed with the direct method, comparably to this work. This figure shows the most promising UV tracers of metallicity.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Top panels: comparison of the high-ionization regions T  e (O III] λ1666/[O III] λ5007) estimated from the hybrid UV–optical ratio, using n  e ([Ar IV]) (blue squares on the left) or n  e (N IV]) (green crosses on the right), as a function of T  e ([O III] λ4363/[O III] λ5007). The uncertainties on the displayed quantities are shown in both axes. In general, the values are roughly in agreement with the dashed black line, which represents the 1:1 relation. Bottom panels: difference in dex between T  e ([O III] λ4363/[O III] λ5007) and T  e (O III] λ1666/[O III] λ5007), keeping same symbols and colors as in the top panel. The colored dashed and dotted horizontal lines in the main and minor panels, respectively, show the median values of the displayed quantities.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Top panel: comparison of the ﹩\mathrm{log}(U)﹩ estimated from low- (S2S3; purple squares), intermediate- (O3O2; green diamonds), and high-ionization regions (Ar4Ar3; orange circles) as a function of 12+log(O/H). The uncertainties on the displayed quantities are shown in both axes. Bottom panel: differences Δ(log U)O3O2−S3S2, in purple, and Δ(log U)O3O2−Ar4Ar3, in orange (we refer to this quantity as Δ(log U)O3O2), revealing significant discrepancies in the range ±1 dex. The colored dashed (in the main panel) and dotted (in the bottom panel) lines indicate the median values. The shaded regions in the bottom panel represent the 68% intrinsic scatter of each distribution, color coded accordingly. This scatter of log(U) values is in line with the presence of a clear ionization structure in the nebular environments of our targets.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Top panels: comparison of 12+log(O/H) from Paper I, with the estimates obtained using the combination of with either n  e ([Ar IV]) or n  e (N IV]), and either T  e ([O III] λ4363/λ5007) or T  e ([O III] λ1666/λ5007), as indicated in the legend, as a function of the stellar mass. For clarity reasons, the optical and hybrid optical–UV measurements of 12+log(O/H) are shown on the left and right, respectively, while 12+log(O/H) from Paper I is shown in both panels. The uncertainties on the displayed quantities are shown in both axes. Bottom panels: difference in dex between Paper I 12+log(O/H) and the other estimates, keeping the same symbols and colors as in the top panel.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Comparison of optical and UV metallicities, comparing Paper I 12+log(O/H) with the exclusively UV He2-O3C3 and Si3-O3C3 calibrations proposed by B20, shown as blue stars and magenta pluses. The uncertainties on the displayed quantities are shown in both axes. The dashed black line indicates the 1:1 relation. The dotted–dashed blue and magenta lines show the best fits of the 12+log(O/H)UV as a function of the optical 12+log(O/H), as reported in the legend. The blue and magenta dashed and dotted lines represent the 1σ and 2.6σ around each best fit.