adsabs/AstroCLIMB huggingface dataset:
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: Total X-ray absorbing gas column (N H) versus dust reddening E(B − V) for the host galaxy and AGN. The contribution to the obscuration from the host galaxy is shown by the black stars; their N H values are those expected based on the average central values of E(B − V) and the SMC gas-to-dust ratio as indicated by the shaded blue region. The N H contribution from the host could be lower if the Galactic gas-to-dust ratio (in gray) is assumed. For CID_473, CID_1210 and CID_1245, their total obscuration is indicated by the red stars. These include the contribution of the host galaxy and inner obscuring structure (i.e., torus). For comparison, we plot a local AGN sample Maiolino et al. (2001) in gray.
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: 2D decomposition of CID_473 using the F444W filter. The pixel scale is 0.″03 pixel−1. The panels are as follows: data, model, data minus point source (host galaxy only), normalized residual (data–model/σ), and surface brightness profile. The top row  includes an unresolved point-source component to the model while the bottom row does not. It is apparent that a central component improves the fit.
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: HST/ACS F814W and JWST/NIRCam (F115W, F150W, F277W, and F444W) images of three X-ray AGNs in COSMOS-Web exhibiting galaxy-scale dust lanes. The axes are labeled in units of arcseconds, while the physical scale is also shown in the top panels. The galaxies are ordered by increasing redshift (shown in the top panels) from left to right.
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: Host galaxy fluxes and best-fit SEDs using MICHI2 (red) and CIGALE (black). The observed fluxes are given in red with 1σ uncertainties. The unattenuated model SED from CIGALE is shown in blue. The JWST/NIRCam filters are shown in the top panel.
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: Decomposed AGN JWST fluxes (circles) and best-fit SED (blue = unattenuated; black = attenuated) from Lyu et al. (2017). Open symbols indicated upper limits on AGN emission.
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: Color images (RBG, top panels) generated by using the F444W, F277W, and F115W filters. Reddening maps E(B − V) are shown in the bottom panels, which are binned by a factor of 2, and thus have a pixel scale of 0.″06. The axes of all images are given in arcseconds.
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: X-ray AGNs in CEERS with prominent galaxy-scale dust lanes in the bluer filters (F150W and F200W). Each row displays the individual JWST images for each filter for a single source. Photometric redshifts are as labeled. The axes are given in arcseconds.
Paper: Resolving Galactic-scale Obscuration of X-Ray AGNs at z ≳ 1 with COSMOS-Web
Authors: John D. Silverman, Vincenzo Mainieri, Xuheng Ding, Daizhong Liu, Knud Jahnke, Michaela Hirschmann, Jeyhan Kartaltepe, Erini Lambrides, Masafusa Onoue, Benny Trakhtenbrot, Eleni Vardoulaki, Angela Bongiorno, Caitlin Casey, Francesca Civano, Andreas Faisst, Maximilien Franco, Steven Gillman, Ghassem Gozaliasl, Christopher C. Hayward, Anton M. Koekemoer, Vasily Kokorev, Georgios Magdis, Stefano Marchesi, Robert Michael Rich, Martin Sparre, Hyewon Suh, Takumi Tanaka, Francesco Valentino
Figure caption: 2D decomposition of CID_1245 and CID_1210 using the F444W filter. The pixel scale is 0.″03 pixel−1. The panels are as follows: data, model, data minus point source (host galaxy only), normalized residual (data–model/σ), and surface brightness profile. All cases include an unresolved point-source component to the model.
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: Top: core-envelope shear S ce, defined as the ratio between the radial shear and a solar latitudinal shear (assumed to be 0.2), represented in background colors. Bottom: the fractional change in the angular momentum content between cores of calibrated models and fully decoupled models F couple, a diagnostic for angular momentum transport. Circles are scaled in size to observed starspot fraction with the color convention from Figure 2. Shear ratios greater than 200 on the top plot are represented as the same color to improve visibility. Overactivity is seen for models with both strong internal shears (top, S ce ≳ 50) and large integrated angular momentum fluxes (bottom, F couple ≳ 0.05). Inset: evolution of core angular momentum for 1.0, 0.8, and 0.65 M ⊙ fiducial rotational models (solid) and fully decoupled models (dotted). By Praesepe age, the two higher mass models depart from full decoupling and show significant angular momentum exchange, but the 0.65 M ⊙ model does not.
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: The Praesepe rotation period distribution, indicating observed rotation and spot anomalies. Symbol sizes are scaled to the measured starspot filling fraction, and colors correspond to the logarithm of the ratio between the observed spot fraction and predictions from a standard Rossby scaling (Equation (4) from Cao & Pinsonneault 2022). The blue line indicates a fit to NGC 6811 (1 Gyr) after transforming temperatures from Curtis et al. (2020) to our spotted temperature system using Praesepe stars in common. Points lying on the blue line appear to stall in their surface spin down between the ages of Praesepe and NGC 6811. The purple line instead indicates the expected rotation periods of these stars by NGC 6811 age assuming solid-body rotation. Inset: the rotational evolution of cores (dashed) and envelopes (solid) for spotted models at 1.0 and 0.8 M ⊙, showing large radial shears in the 0.8 M ⊙ model at Praesepe age.
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: Absolute K-band magnitude for each star plotted against Gaia B  P  − R  P  color, points scaled according to measured starspot filling fraction. Gray crosses indicate binaries, cyan circles are stars for which there were no matches to rotation periods (Rebull et al. 2017), and black circles are the single stars in these open cluster samples. Histograms are shown for populations of binaries (gray), stars with no reported rotation periods (blue), and single stars with measured periods (black). The rotation period completeness is high with no trends in rotation nondetections, particularly near the overactive stars (1.5 < B  P  − R  P  < 1.9).
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: The time evolution of core-envelope shear is plotted for models launched from the Upper Sco rotational sequence that reproduce the observed rotation at Praesepe age and metallicity. Contours of core-envelope shear ratios are shown ranging from 10 to 50. The hatched region corresponds to models where the integrated angular momentum flux from core to envelope is relatively weak (the A.M. coupling diagnostic is ≤0.05). The region bounded by a brown dashed contour represents a standard starspot saturation criterion (Cao & Pinsonneault 2022). The region with shear ratios >50 and significant angular momentum exchange is interpreted to be the locus of shear-enhanced magnetism in stars. The timescale for shear-enhanced magnetism varies strongly with T eff, from ∼100 Myr at 4900 K to ∼700 Myr by 4500 K and ∼5 Gyr by 4100 K.
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: Starspot filling fractions derived from the fit to APOGEE DR17 spectra are reported for single stars with rotation periods in Praesepe. Red error bars are 3σ outliers in the Ro–fspot relation (Equation (4) from Cao & Pinsonneault 2022) after accounting for total population dispersion, including inclination and cyclic variation effects. Gray error bars are stars in the same color range as possibly spuriously overactive stars in M67 (Cao & Pinsonneault 2022) and should be interpreted with caution. Overactive stars in Praesepe are tightly clustered; 15 of 21 stars between 3950 < T eff < 4410 K are >3σ discrepant in activity. Inset: the f spot–Rossby diagram is shown with upper limits represented as triangles.
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: Three sets of gyrochrones launched from the Upper Sco rotation distribution (at 7.5, 50, 92.5th percentiles, corresponding to orange, blue, and green, respectively) are shown in each plot against observed cluster member sequences including binaries. Observed periods are colored according to matching bins (at 0–15th, 15–85th, and 85–100th percentiles), and an additional black outline is displayed on stars that comprise our single star sample. An additional gyrochrone at the 65th percentile is shown in black against the single star sequence of each cluster. Top: the Pleiades rotation distribution and best-fit gyrochrones. Bottom: the Praesepe rotation distribution and best-fit gyrochrones.
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: Marginalized 2D probability distributions for each gyrochronology fit parameter described in Appendix A.2. Convergence is seen in all parameters, with a burn-in of 300 step evaluations and a total chain length of 2100 steps. Final parameters are as follows: f  k  = 9.79 ± 0.37, ω crit = (3.466 ± 0.085) × 10−5 rad s−1, ﹩{\tau }_{\mathrm{ce},\odot }=\left(2.66\pm 0.36\right)\times {10}^{7}\,\mathrm{yr}﹩, and α = −11.8 ± 1.0.
Paper: Core-envelope Decoupling Drives Radial Shear Dynamos in Cool Stars
Authors: Lyra Cao, Marc H. Pinsonneault, Jennifer L. van Saders
Figure caption: Color–magnitude diagram with Gaia DR3 synthetic photometry in dereddened V − K against absolute V-band photometry. The points indicate the Pleiades (cyan), Praesepe (black), and Praesepe overactive (red) stars. The lines show standard color–magnitude relations (Cao & Pinsonneault 2022) for the Pleiades (cyan) and Praesepe (black). Inset: B − V color anomaly evaluated at fixed K-band magnitude, plotted against dereddened V − K color. Large B − V color anomalies are observed to occur in stars with large surface spot filling fractions.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Left panel: a few representatives of the time series of the annual daily Lyα irradiance for solar cycle maximum (1947, 1969, 1989, and 2014) and minimum (1986, 1996, 2008, and 2019). Right panel: the autocorrelation function corresponding to the left panel that was used to estimate the synodic rotation period. The red curves represent the significant first secondary maximum for the autocorrelation coefficients fitted by the Gaussian function; the horizontal lines in the plot correspond to 95% (lower solid gray) and 99% (upper dashed gray) confidence levels.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Panel (a): the daily Lyα irradiance in 1957 and the trend in this series. Panel (b): the autocorrelation function corresponding to panel (a). Panel (c): the detrending irradiance in 1957. Panel (d): the autocorrelation function corresponding to the detrending irradiance (black curve) and the smoothed irradiance (gray curve), and the red curves represent the third secondary maximum for the autocorrelation coefficients fitted by the Gaussian function. The horizontal lines in panels (b) and (d) correspond to 95% (lower solid gray) and 99% (upper dashed gray) confidence levels, respectively.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Temporal variation of the sidereal rotation periods of solar transition region during 1947–2022. The scatters are the raw sidereal rotation periods obtained by the autocorrelation method. The black straight line is the regression-fitted result of the sidereal rotation periods. The black curve is the 5 yr smoothed sidereal rotation period. The vertical dashed gray and dotted gray lines represent solar cycle minimum and maximum, respectively.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Panel (a): the daily Lyα irradiance in 1954 and the trend in this series. Panel (b): the autocorrelation function corresponding to panel (a). Panel (c): the detrending irradiance in 1954. Panel (d): the autocorrelation function corresponding to panel (c), and the red curves represent the significant first secondary maximum for the autocorrelation coefficients fitted by the Gaussian function. The horizontal lines in panels (b) and (d) correspond to 95% (lower solid gray) and 99% (upper dashed gray) confidence levels, respectively.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Panel (a): the daily Lyα irradiance in 1977 and the trend in this series. Panel (b): the autocorrelation function corresponding to panel (a). Panel (c): the detrending irradiance in 1977. Panel (d): the autocorrelation function corresponding to the detrending irradiance, and the red curves represent the third secondary maximum for the autocorrelation coefficients fitted by the Gaussian function. The horizontal lines in panels (b) and (d) correspond to 95% (lower solid gray) and 99% (upper dashed gray) confidence levels, respectively.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Panel (a): the daily Lyα irradiance in 1969 and the trend in this series. Panel (b): the autocorrelation function corresponding to panel (a). Panel (c): the detrending irradiance in 1969. Panel (d): the autocorrelation function corresponding to the detrending irradiance, and the red curves represent the significant first secondary maximum for the autocorrelation coefficients fitted by the Gaussian function. The horizontal lines in panels (b) and (d) correspond to 95% (lower solid gray) and 99% (upper dashed gray) confidence levels, respectively.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Same as Figure 7, but for the descending phase (1950, 1960, 1995, and 2017) and the ascending phase (1955, 1980, 2013, and 2020) of solar cycles.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: The daily composite Lyα from 1947 February 14 to 2023 February 20. The vertical dashed gray lines indicate the time of minimal solar activity.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Same as Figure 2, but for 1948.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: The cross-correlation coefficients between the sidereal rotation period and the yearly sunspot numbers. Upper panel: the black solid curve is the result calculated from the two 5 yr smoothed data sets, and the black dashed curve is the result calculated from the two raw data sets. Lower panel: same as the upper panel, but for the detrending data sets. The bold dashed black vertical lines are the maximum value of the coefficients.
Paper: Temporal Variation of the Rotation in the Solar Transition Region
Authors: Xiaojuan Zhang, Linhua Deng, Yu Fei, Chun Li, Xinan Tian
Figure caption: Panel (a): the sidereal rotation periods in the solar transition region from 1947 to 2022 and the trend in this series. Panel (b): the autocorrelation function corresponding to the raw sidereal rotation periods (dashed black curve) and the 5 yr smoothed ones (solid black curve). Panel (c): detrending sidereal rotation periods in the solar transition region for 1947–2022. Panel (d): same as panel (b), but for the detrending sidereal rotation periods. The horizontal lines in panels (b) and (d) correspond to 95% (lower solid gray) and 99% (upper dashed gray) confidence levels, respectively.
Paper: Early Results from GLASS–JWST. XXI. Rapid Asembly of a Galaxy at z = 6.23 Revealed by Its C/O Abundance
Authors: Tucker Jones, Ryan Sanders, Yuguang Chen, Xin Wang, Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Alan Dressler, Emiliano Merlin, Diego Paris, Paola Santini, Pietro Bergamini, A. Henry, Erin Huntzinger, Themiya Nanayakkara, Kristan Boyett, Marusa Bradac, Gabriel Brammer, Antonello Calabró, Karl Glazebrook, Kathryn Grasha, Sara Mascia, Laura Pentericci, Michele Trenti, Benedetta Vulcani
Figure caption: The ﹩\mathrm{log}({\rm{C}}/{\rm{O}})﹩ and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ values of our target z = 6.23 galaxy (red star) compared to other objects compiled from literature: Milky Way halo and disk stars (light-green crosses; Gustafsson et al. 1999; Akerman et al. 2004; Fabbian et al. 2009; Nissen et al. 2014); damped Lyα absorbers (DLAs; pink triangles; Cooke et al. 2017); local dwarf galaxies (Berg et al. 2016, 2019; Peña-Guerrero et al. 2017; Senchyna et al. 2017); and z = 0 H II regions (Tsamis et al. 2003; Esteban et al. 2004, 2009, 2014, 2017; García-Rojas et al. 2004, 2005, 2006; Peimbert et al. 2005; García-Rojas & Esteban 2007; López-Sánchez et al. 2007; Toribio San Cipriano et al. 2016, 2017) (z ∼ 0; cyan squares); high-redshift galaxies near cosmic noon (z ≃ 1.5–3.5) (orange pentagons; Fosbury et al. 2003; Erb et al. 2010; Christensen et al. 2012; Bayliss et al. 2014; James et al. 2014; Stark et al. 2014; Steidel et al. 2016; Vanzella et al. 2016; Amorín et al. 2017; Berg et al. 2018; Mainali et al. 2020; Matthee et al. 2021; Rigby et al. 2021; Iani et al. 2023); and a galaxy at z = 8.5 from Arellano-Córdova et al. (2022) (AC22: orange circle). The ﹩\mathrm{log}({\rm{C}}/{\rm{O}})﹩ ratio from pure core-collapse SNe enrichment is marked with violet shading. This C/O range was calculated using the Z * = 0.05Z ⊙ and 0.2Z ⊙ values from the Nomoto et al. (2013) yield tables assuming a Salpeter (1955) initial mass function. The C/O abundance ratio of this galaxy is at the lower envelope of other low-metallicity sources, consistent with pure SNe II enrichment and implying a young stellar population without significant enrichment from AGB stars. Note: for the z = 0 H II regions, C/O was measured from recombination lines (RLs). We plot O/H derived using the collisionally excited line (CEL) T e-method to match the O/H scale of the z ∼ 0 dwarf galaxy and z ≳ 2 samples. We assume that the abundance discrepancy factor is the same for C and O (e.g., Toribio San Cipriano et al. 2017), such that C/O derived from RLs and CELs can be fairly compared.