adsabs/AstroCLIMB huggingface dataset:
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Temperature–rotation period diagrams. Top: apparently single stars in Blanco 1 and benchmark comparison clusters. Bottom left: single and multiple stars in Blanco 1. Bottom right: Blanco 1 and comparison sample stars. For Blanco 1, the circular marks are core stars that fall within the tidal radius estimated by X. Pang et al. (2021), and the square marks are those that are outside the tidal radius, i.e., in the tidal tails. The effective temperatures are derived from Gaia DR2 G BP − G RP colors using an empirical relation derived by J. L. Curtis et al. (2020). The gray dashed lines in the bottom panels indicate the gyrochrone of Blanco 1, with the shaded region being the ±1.25 day band where we consider a star to fall within the gyrochrone.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: H-R diagrams of the open cluster Blanco 1 (left: core, center: tidal tails) and the comparison sample of field stars (right). Stars with measured rotation periods are plotted in circular marks of various colors, and those whose light curve shows no identifiable rotation signal are plotted in square purple marks. The gray triangular marks are the stars without valid light curves in the sample.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Histograms comparing the Blanco 1 member candidates (orange lines) and the selected comparison sample of field stars (purple lines). Top left: parallax histograms. The Blanco 1 candidates shows a clustering in parallax, while the comparison sample is evenly distributed. Top and bottom right: proper motion histograms. The Blanco 1 candidates show a sharp peak in proper motion space, and they are plotted on a different scale (right y-axis) for convenience. The comparison sample excludes those peaks; see also Figure 5. Bottom left: Gaia DR3 G-magnitude histograms. The distributions for Blanco 1 candidates, and the comparison sample closely match.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Gaia DR3 multiplicity indicators for Blanco 1 member candidates. Stars that are apparently single appear in gray. The acronyms in the legend are as follows. HR: on the binary sequence in the H-R diagram. RV: above the cutoff in RV uncertainty. RUWE: above the cutoff of the Gaia DR3 RUWE parameter.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Blanco 1 members in Galactic Cartesian coordinates XYZ, as determined by X. Pang et al. (2021). The dashed gray circle indicates the nominal tidal radius determined by X. Pang et al. (2021), and the black arrow within the circle is the projected direction to the Sun. The circular orange marks are the stars with an actually measured rotation period, and the triangular gray marks are those without a measured period.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Blanco 1 core members in Galactic Cartesian coordinates XYZ, as determined by X. Pang et al. (2021). The dashed gray circle indicates the nominal tidal radius determined by X. Pang et al. (2021). The circular orange marks are the stars with a measured rotation period, and the triangular gray marks are those without a measured period.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Sky charts for Blanco 1 cluster candidate members identified by X. Pang et al. (2021). The charted positions are from Gaia DR3. Left: full view of Blanco 1. Right: zoomed-in view of the cluster core. The circular orange marks are the stars within the tidal radius of the cluster, and the square magenta marks are those outside of the tidal radius.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Posterior distribution for the contamination ratio of the tidal tail candidates in Blanco 1. The shaded regions indicate the 2σ and 3σ intervals starting from zero, with the respective upper limits highlighted in black lines.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Saturation Test 2. J1025+3622 fits with ﹩\mathrm{log}({N}_{\mathrm{Si}\,\mathrm{II}})﹩ fixed to different values in the saturated regime (14.5, 15.0, and 16.0). For these test fits, the covering fractions, column densities associated with other elements, and v min are fixed at the best-fit values for J1025+3622, while b is allowed to vary. Top: The curve of growth for Si II λ1260 for these test fits (i.e., the black curves), pinpointing three locations in the saturated zone: the best fit in purple, a lower column density in pink, and a higher column density in orange. The light purple shading corresponds to the saturated regime. Bottom: The models corresponding to these fixed Si II column densities compared with the observed spectrum for J1025+3622. As shown here, we are able to distinguish between the accuracy of these fits to the data even though they all correspond to saturated absorption. This demonstrates that our fitting procedure is capable of constraining the column density of saturated lines.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Saturation Test 2 (cont.). Similar to Figure 4, except ﹩\mathrm{log}({N}_{{\rm{O}}\,{\rm{I}}})﹩ is fixed to different values in the saturated regime (15.4, 15.8, and 16.5), while ﹩\mathrm{log}({N}_{\mathrm{Si}\,\mathrm{II}})﹩ is fixed to 15.0 (the best-fit value for this galaxy). Once again, b is allowed to vary. This shows that, even for a single saturated line, we can still distinguish between these fits when compared with the data. This further supports our ability to constrain the column densities for saturated lines.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Simultaneous one-component fits (solid purple line) to the LIS features in the high-S/N, high-spectral-resolution CLASSY spectrum for J1150+1501 (solid black line). Lines not included in the fit but predicted using the fit parameters are shown as dashed purple line profiles. The systemic wavelengths of the LIS absorption lines are marked by vertical dotted lines, while the line’s trough (v min) is denoted by the solid black ticks. Milky Way features, denoted by vertical dashed magenta lines, were not included in the fit. Figures presenting the fits for the other CLASSY galaxies are included in Appendix E.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: An example of the stacked and reduced 21 cm H I profile from the HICLASS observations of J1132+5722, shown in black. A smoothed version of this signal is overplotted in gray. The bounds of integration used to calculate S H I , chosen by eye to include the full emission profile, are shown by dashed pink lines, while the area associated with S H I  is shaded in light yellow. The solid pink line denotes the systemic velocity of the galaxy (v = 0 km s−1). Similar plots for the other CLASSY galaxies with H I observations are in Appendix A.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: The velocity offsets of the strongest line for each ion (O I λ1302: red points, C II λ1334: green points, S II λ1254: yellow points, Si II λ1260: pink points, Al II λ1670: purple points). The x-axis lists the galaxies in our sample, ordered by the average value of these points. Top: The difference in velocity compared to O I, for those where it is measured. Overall, this shows that the velocity offsets are generally consistent between these ions, which is expected if they were produced by the same clouds of gas. This further motivates the use of a single component of gas to simultaneously fit this series of absorption lines.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Comparing our one-component fit results (y-axis) with the previous two-component fits from X. Xu et al. (2022) (x-axis) for CLASSY. Left: v min vs. the outflow velocities from X. Xu et al. (2022). The dashed line corresponds to a one-to-one relationship. The filled points correspond to the one-component sample while the empty points are the multi-component sample. The points with a central dot correspond to the galaxies with at least one unsaturated line in their fit. The points are color-coded by the Doppler broadening. Right: ﹩\mathrm{log}({N}_{\mathrm{Si}\,\mathrm{II}})﹩ vs. the column densities of the Si II outflows as reported by X. Xu et al. (2022). Overall, we see good agreement for galaxies that have wind-dominated absorption profiles (large v out), while our one-component fits extend to smaller velocities for galaxies with ISM-dominated profiles.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Saturation Test 1. We performed our MC least-squares fitting procedure on a series of 1000 models of saturated Si II λ1260 absorption across a grid of input parameters (b, ﹩\mathrm{log}(N)﹩, C  f ), adding noise and assuming a resolution similar to those typical of the CLASSY observations. This figure shows a histogram of the differences between the results of these fits, ﹩\mathrm{log}({N}_{{\rm{fit}}})﹩, and the actual values, ﹩\mathrm{log}({N}_{{\rm{init}}})﹩. Since this distribution is centered on zero and is relatively symmetric, it demonstrates that our MC approach is capable of constraining ﹩\mathrm{log}(N)﹩ for saturated lines.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: The simultaneous one-component fit for J1359+5726, a member of the multi-component sample, which requires more than one component to adequately fit the observed LIS absorption. See caption of Figure 6 for details.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Comparing O I and LIS ion fit results: W  λ  (top row), ﹩\mathrm{log}(N)﹩ (middle row), and C  f  (bottom row). The x-axis of all panels corresponds to O I, while the y-axis corresponds to C II, Si II, S II, and Al II. The filled points represent galaxies with R  f  ∼ 1 − C  f  , while the empty diamond points correspond to those with C  f  ∼ 1 and a nonzero R  f . We expect that the difference between these subsets is related to their opacity, with the optically thick lines shown by filled points while the empty diamonds are optically thin, at least based on classifications described in Figure 9 for O I. The galaxies with ≥1 unsaturated line in the fit are distinguished by a point in their center. The W  λ  values are measured for individual lines (C II λ1334, S II λ1260 and λ1526, S II λ1254 and λ1259, and Al II λ1671), while ﹩\mathrm{log}(N)﹩ and C  f  are determined by all lines for that ion that were included in the fit. The linear fits to the solid points are shown in each panel by the solid black line (pink/blue to differentiate for S II and Si II W  λ  panels) while the one-to-one relationship is shown as a dotted line. The measurements shown in this figure and used in these fits are limited to those with S/N > 1. The Pearson correlation coefficients (R) and their associated p-values are listed in the panels.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Global properties of the CLASSY galaxies (﹩\mathrm{log}({M}_{\star })﹩, SFR, r 50, M 1500, and M H I) vs. the fitted column densities for O I, Si II, C II, S II, and Al II, color-coded by b from our fits. The filled points correspond to measurements for the galaxies in the one-component sample, while the empty points are for those in the multi-component sample. Galaxies with at least one unsaturated line are distinguished by a black dot at their center. The solid black line is the linear fit to all points (filled + empty), with uncertainties represented by the light gray curves. From these panels, we find the strongest correlations to be with O I and C II column densities and these galactic properties. In general, we show that the galaxies with higher column densities of absorbing gas tend to be those that are more massive, have higher SFRs, are more compact, and are intrinsically brighter.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: Column densities of neutral and low-ionization metals vs. H I column densities measured from Lyα emission (W. Hu et al. 2023). The points are color-coded by gas fraction, μ, or are white for galaxies lacking 21 cm detections. The central black dots correspond to the galaxies with at least one unsaturated line in their fit. The solid black lines are linear fits to each panel, while the light gray lines correspond to fits from 1000 MC variations to the measurements based on their uncertainties. This figure shows a lack of a significant trend between the O I and Lyα-derived H I column densities, at least for this relatively small range in ﹩\mathrm{log}({N}_{{\rm{H}}\,{\rm{I}}}^{\mathrm{Ly}\alpha })﹩. The trends in the middle and lower panels, however, have statistically significant correlations at a ≳95% confidence interval based on their Pearson correlation p-values (listed at the bottom of each panel). Of these three panels, Si II exhibits the strongest correlations, both with ﹩{N}_{{\rm{H}}\,{\rm{I}}}^{\mathrm{Ly}\alpha }﹩ and μ. Since O I and Si II trace similar populations of gas (see Section 4), a trend may still exist between the O I column densities and N H ILy α.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: The ﹩\mathrm{log}({M}_{{\rm{H}}\,{\rm{I}}}﹩/M ⋆) measurements for the 27 CLASSY galaxies with H I 21 cm detections and the eight galaxies with nondetections (shown as upper limits) as a function of the stellar mass (purple diamonds). Comparing our measurements with those from the LVL (V. Parkash et al. 2018), ALFALFA (A. Saintonge et al. 2011; N. Maddox et al. 2015), and SHIELD surveys (K. B. W. McQuinn et al. 2021), we find that the majority of CLASSY galaxies are gas-rich. The green stars correspond to the low-mass star-forming galaxies Pox 186 (M. R. Corbin & W. D. Vacca 2002; A. Begum & J. N. Chengalur 2005; N. R. Eggen et al. 2021), Leo P (K. B. W. McQuinn et al. 2015), and DDO 210 (D. A. Hunter et al. 2012). Six CLASSY galaxies are particularly gas-poor compared to the rest of the sample: J0036–3333 (μ = 0.297), J0127–0619 (μ = 0.208), J0808+3948 (μ < 0.087), J0938+5428 (μ < 0.078), J0942+3547 (μ < 0.091), and J1359+5726 (μ < 0.253).
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: The O I covering fractions vs. O I λ1302 residual fluxes, color-coded by ﹩\mathrm{log}({N}_{{\rm{O}}\,{\rm{I}}})﹩. This plot shows two main subsets: those that roughly follow R  f  ∼ 1 − C  f  and those with C  f  ≈ 1 and relatively large R  f  values. These seem to correspond to lines in the optically thick and optically thin regimes, respectively. This is evidenced by the correlation that column density seems to have with these measurements: the galaxies with optically thin O I tend to be those with low O I column densities, often with log(N O I<15.5.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: J0127–0619: The common name of J0127–0619 is Mrk 996. This galaxy is known to have complex emission line kinematics, a large Wolf–Rayet (WR) population, and a high electron density within its inner core region (T. X. Thuan et al. 1996; B. L. James et al. 2009; E. Telles et al. 2014). Galaxies with WR spectral features often have more highly ionized ISM than other star-forming galaxies (e.g., J. Brinchmann et al. 2008). Additionally, its broad FWHM (∼95 km s−1) could be further evidence of WR stars and/or an AGN. Using a large sample of AGN from the xGASS and ALFALFA surveys, S. L. Ellison et al. (2018) found that low-mass (﹩\mathrm{log}{M}_{\star }\lt 9.6﹩) galaxies with AGN are typically H I-poor. Together, these factors indicate that J0127–0619's low gas fraction (μ ∼ 0.2) is the result of its extremely ionized conditions and high-energy sources.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: The residual fluxes R  f  of the lines for each ion (O I λ1302: red points, C II: green points, S II: yellow points, Si II: pink points, Al II: purple points). The x-axis lists the galaxies in our sample with at least 1 O I line in the fit, ordered by R  f (O I). Top: The difference between R  f (line) and R  f (O I). Overall, this shows how the residual fluxes of different ions relate to that of O I.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: The median gas-phase fractions ﹩({M}_{X}^{{\rm{gas}}}/{M}_{X}^{{\rm{tot}}})﹩ of the metals in our analysis for the CLASSY galaxies, as estimated from their depletion factor F ⋆ and the empirical trends from E. B. Jenkins (2009), A. De Cia et al. (2016), and C. Konstantopoulou et al. (2022). This shows that the total fraction of carbon in the gas (vs. in the dust) is most similar to that of oxygen, which may explain why C II properties have a stronger correlation with O I compared to the other ions.
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: The FWHM of the 21 cm profile as a function of the velocity offset of the LIS absorption lines, color-coded by the total SFRs. This plot relates kinematic information as measured from the 21 cm emission and the LIS absorption and shows a loose anticorrelation between the FWHM21 cm and v min. This indicates that the galaxies with stronger outflows of neutral and LIS gas (i.e., more negative values for v min) also tend to have broader 21 cm H I profiles—indicating more organized gas flows—and higher star formation rates.