adsabs/AstroCLIMB huggingface dataset:
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Left: luminosity functions for all non-OOB stars in our sample, expressed as the number of stars with luminosity greater than or equal to L, N(≥ L). Dashed/solid lines include/exclude low-L stars, respectively. Black lines are for stars at all temperatures, while the luminosity functions for RSGs, YSGs, and BSGs are correspondingly colored. Right: same, but normalized to unity at ﹩\mathrm{log}L/{L}_{\odot }=4.5﹩. In both panels, the slopes of the luminosity functions vary, with the YSG luminosity function becoming notably flatter above ﹩\mathrm{log}L/{L}_{\odot }\approx 5﹩.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption:  G − K  S  vs. J − K  S  color–color diagram for the non-OOB Y21 stars, colored by our newly derived ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ values. The horizontal black line shows the G − K  S  color of a star that is at the completeness limit for both Gaia low-resolution spectroscopy and 2MASS K  S . A star at the Gaia completeness limit but bluer than this line will not be detected by 2MASS; i.e., they are just bright enough in the optical for Gaia spectroscopy, but not enough in the infrared to have a derived temperature via the J − K  S  method. Many massive stars in the Local Group satisfy this criterion.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Effective temperature scale for the LMC cool supergiants in our sample; temperatures for stars later than K0 are plotted in linear scaling in the right panel. Overplotted are effective temperature scales from the literature: the temperature scales for solar (solid line) and SMC (dashed line) AFG supergiants from Evans & Howarth (2003) are shown in green, the scale for LMC GKM supergiants from Tabernero et al. (2018) is shown in orange, and the LMC RSG effective temperature scale from Levesque et al. (2006) is shown in blue.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: The difference between the observed and corrected J − K  S  color and the value of J − K  S  implied using our machine-learned ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ values and inverting the N12 polynomial, ΔJ − K  S , as a function of the observed J-band magnitude, colored by our derived ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ values.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Results from a greedy search over features averaged over five folds of the training set for the Bayesian RR trained on an interactively grown subset of features. The blue line and errors respectively show the mean and standard deviation of ﹩{d}_{M,95}^{2}﹩ across five folds of the training set. Green and red show the percentage of residuals within 1 and 2σ of their expected values, respectively.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Sampled Gaia spectra of the brightest star in each 0.05 dex–wide bins in ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ between 3.55 and 4.05. The spectra are color coded by their effective temperature as indicated by the color bar.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Top left: KDE of the H-R diagram, ρ HR. Low-luminosity RSGs are the most common stars in the sample. Bottom left: ρ HR normalized by the KDE of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩, ρ  T ; equivalent to the differential luminosity function as a function of temperature. Lower-luminosity stars are more common, but the luminosity function flattens at ﹩\mathrm{log}{T}_{\mathrm{eff}}\approx 3.8﹩. Top right: ρ HR normalized by the KDE of ﹩\mathrm{log}L/{L}_{\odot }﹩, ρ  L ; brighter regions are temperatures with longer lifetimes. The RSG branch can clearly be seen, but the YSG and BSG lifetimes relative to the RSG phase increase at high luminosity. Bottom right: ρ HR normalized by ρ  L  ρ  T . Brighter regions show overdensities in the H-R diagram, and dark regions show underdensities.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: Similar to the bottom right panel of Figure 11, after subtracting and dividing by the median value. The one-dimensional KDEs of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ and ﹩\mathrm{log}L/{L}_{\odot }﹩ are shown above and to the right of the plot, respectively. Regions with colors close to black contain roughly as many stars as one would expect by simply drawing values from each one-dimensional KDE, while regions in red/blue have fewer/more stars. We postulate that the region in blue contains post-RSGs; the white points are the positions in the H-R diagram of the recently discovered FYPSs, which are putative post-RSGs (Dorn-Wallenstein et al. 2022). The cross-hatched region shows the minimum-luminosity boundary of the sample used to compute the KDE.
Paper: Physical Properties of 5000 Cool Large Magellanic Cloud Supergiants with Gaia XP Spectra: A Detailed Portrait of the Upper H-R Diagram Hints at Missing Supernova Progenitors
Authors: Trevor Z. Dorn-Wallenstein, Kathryn F. Neugent, Emily M. Levesque
Figure caption: A summary of the performance of each regressor we experimented with on both temperature and luminosity simultaneously. The two panels in the top left show the predicted versus actual values of each star the test set for ﹩\mathrm{log}L/{L}_{\odot }﹩ (top left) and ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ (center left). The bottom left panel shows the individual squared Mahalanobis distance d  M  2 for each point as a function of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩. Dashed/dashed–dotted/dotted lines indicate 64/95/99.7% confidence levels for a χ 2 distribution with two degrees of freedom, corresponding to 1/2/3σ differences between the observed and true values. The top right panel shows the histogram of d  M  2 and the bottom right panels show the ﹩{d}_{M,95}^{2}﹩ values for each regressor. This panel also serves as a legend to map between the regressors and the colors of the corresponding points in the other panels.
Paper: Probing the Galactic Diffuse Continuum Emission with COSI
Authors: Christopher M. Karwin, Thomas Siegert, Jacqueline Beechert, John A. Tomsick, Troy A. Porter, Michela Negro, Carolyn Kierans, Marco Ajello, Israel Martinez-Castellanos, Albert Shih, Andreas Zoglauer, Steven E. Boggs
Figure caption: Observed intensity toward the inner Galaxy. The blue data points are for COSI, and the error bars are 1σ statistical only. Upper limits are plotted at the 95% confidence level. The salmon data points are for INTEGRAL/SPI, and the green data points are for COMPTEL, with the error bars on both measurements including statistical and systematic uncertainty. The gray curves show predictions for our three primary GALPROP models, as specified in the legend. The gray band shows the full range spanned by the six GALPROP models from Porter et al. (2021), which includes the SA100-F98 model.
Paper: Probing the Galactic Diffuse Continuum Emission with COSI
Authors: Christopher M. Karwin, Thomas Siegert, Jacqueline Beechert, John A. Tomsick, Troy A. Porter, Michela Negro, Carolyn Kierans, Marco Ajello, Israel Martinez-Castellanos, Albert Shih, Andreas Zoglauer, Steven E. Boggs
Figure caption: The black data points show the continuum emission extracted from Beechert et al. (2022). The error bars are statistical only. The colored bands show the expected count rates for three different GALPROP models of the Galactic diffuse emission. We note that the GALPROP models do not include the line emissions. The predictions are based on MEGAlib simulations, which closely replicate the 2016 COSI observations (i.e., detector and pointing on the sky). The dark and light regions show the 1σ and 2σ statistical uncertainties, respectively.
Paper: Probing the Galactic Diffuse Continuum Emission with COSI
Authors: Christopher M. Karwin, Thomas Siegert, Jacqueline Beechert, John A. Tomsick, Troy A. Porter, Michela Negro, Carolyn Kierans, Marco Ajello, Israel Martinez-Castellanos, Albert Shih, Andreas Zoglauer, Steven E. Boggs
Figure caption: Atmospheric correction factor ratio for an off-axis angle of 44°. We consider a power-law (PL) spectral model with different spectral indices, as specified in the legend, as well as the model of the Galactic diffuse (SA100-F98) from the simulations.
Paper: Probing the Galactic Diffuse Continuum Emission with COSI
Authors: Christopher M. Karwin, Thomas Siegert, Jacqueline Beechert, John A. Tomsick, Troy A. Porter, Michela Negro, Carolyn Kierans, Marco Ajello, Israel Martinez-Castellanos, Albert Shih, Andreas Zoglauer, Steven E. Boggs
Figure caption: The effective area for the Galactic diffuse emission (SA100-F98) calculated from MEGAlib simulations. This represents the average from the total exposure time and is used to convert the observed count rate to flux.
Paper: Direct Statistical Constraints on the Natal Kick Velocity of a Black Hole in an X-Ray Quiet Binary
Authors: Sharan Banagiri, Zoheyr Doctor, Vicky Kalogera, Chase Kimball, Jeff J. Andrews
Figure caption: Schematic of the pre-SN geometry of the binary system, along with the coordinate system being used. Also shown are the kick velocity V  k , the angle θ, the CM kick δ V CM, and the angle the latter makes with the line of sight ι  v . We note that ι  v  is different from the pre-SN inclination angle ι.
Paper: Direct Statistical Constraints on the Natal Kick Velocity of a Black Hole in an X-Ray Quiet Binary
Authors: Sharan Banagiri, Zoheyr Doctor, Vicky Kalogera, Chase Kimball, Jeff J. Andrews
Figure caption: Posterior probability distributions of pre-SN separation, natal kick velocity, and the pre-SN mass for the Maxwellian and uniform velocity models. Uniform mass prior is used in both cases. The shaded regions correspond to 90% credible intervals.
Paper: NuSTAR Hard X-Ray Monitoring of Gravitationally Lensed Quasar RX J1131–1231
Authors: Cora A. DeFrancesco, Xinyu Dai, Mark Mitchell, Abderahmen Zoghbi, Christopher W. Morgan
Figure caption: Unabsorbed flux light curve of all spectra from Nustar, Swift, XMM, and Chandra, where the Chandra flux is from Chartas et al. (2017); all other data were described in this paper. The dotted lines are not physical and only used for the purpose of better reading the individual data points.
Paper: NuSTAR Hard X-Ray Monitoring of Gravitationally Lensed Quasar RX J1131–1231
Authors: Cora A. DeFrancesco, Xinyu Dai, Mark Mitchell, Abderahmen Zoghbi, Christopher W. Morgan
Figure caption: Top: combined XMM-Newton (low energy)/NuSTAR (high energy) fit. The model is represented by the solid red (purple) line overlaying the XMM-Newton (NuSTAR) data. NuSTAR data are shown in two data sets coming from the two focal plane modules FPMA and FPMB. Bottom: residuals of the fit.
Paper: Direct Statistical Constraints on the Natal Kick Velocity of a Black Hole in an X-Ray Quiet Binary
Authors: Sharan Banagiri, Zoheyr Doctor, Vicky Kalogera, Chase Kimball, Jeff J. Andrews
Figure caption: Posterior probability distributions of the kick-velocity dispersion under the Maxwellian model for different mass priors.
Paper: Direct Statistical Constraints on the Natal Kick Velocity of a Black Hole in an X-Ray Quiet Binary
Authors: Sharan Banagiri, Zoheyr Doctor, Vicky Kalogera, Chase Kimball, Jeff J. Andrews
Figure caption: Posterior probability distribution of the pre-SN separation for different mass and velocity distributions. We see that the final posterior is quite insensitive to prior assumptions. For reference, the dashed line shows the post-SN semimajor axis a  f .
Paper: NuSTAR Hard X-Ray Monitoring of Gravitationally Lensed Quasar RX J1131–1231
Authors: Cora A. DeFrancesco, Xinyu Dai, Mark Mitchell, Abderahmen Zoghbi, Christopher W. Morgan
Figure caption: Example Swift spectra. Top left and top right: typical S/N for the Swift spectra (19 and 18, respectively). Bottom left: an example of low-S/N spectrum (4.8) excluded from analysis. Bottom right: an example of high-S/N spectrum (24).
Paper: NuSTAR Hard X-Ray Monitoring of Gravitationally Lensed Quasar RX J1131–1231
Authors: Cora A. DeFrancesco, Xinyu Dai, Mark Mitchell, Abderahmen Zoghbi, Christopher W. Morgan
Figure caption: Model fits for the six Swift/NuSTAR paired observations. Soft X-ray Swift spectra are in black, hard X-ray NuSTAR spectra are in gray, and the model is in red.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: N/O (top left), C/O (top right), C/N (bottom left) as a function of 12 + log(O/H). N/O as a function of C/O (bottom right). The double red circle denotes the measurements of GLASS_150008 based on the stellar photoionization model. The measurements of CEERS_01019 (red square) and GN-z11 (magenta square) are based on the AGN photoionization models, while those based on the stellar photoionization models are shown by the semitransparent red and magenta squares, respectively. The semitransparent magenta dashed lines, magenta triangle, and red crosses are the abundance measurements of GN-z11 by Cameron et al. (2023), GN-z11 by Senchyna et al. (2023), and CEERS_01019 by Marques-Chaves et al. (2023), respectively, all of which are based on the stellar radiation. In the top right panel, C/O ratios of other galaxies in our sample are shown by the gray circles with the error bars. The double circles correspond to the measurements with T e determinations. Mrk996, a WR galaxy, is represented by the black diamonds (Berg et al. 2016; Senchyna et al. 2023). Local galaxies (Izotov et al. 2006; Berg et al. 2016, 2019) and Galactic H II regions (García-Rojas & Esteban 2007) are shown by the gray dots, while the gray curves are the empirical relation of the Galactic stars (Nicholls et al. 2017). The purple circles are dwarf stars in a globular cluster (GC) NGC6752 (Carretta et al. 2005), while those O/H values are taken from Senchyna et al. (2023). The purple stars show abundance ratio distributions of dwarf stars in a metal-rich GC 47 Tuc (Briley et al. 2004; D’Orazi et al. 2010). The pink crosses are carbon-enhanced metal-poor (CEMP) stars (Norris et al. 2013) and nitrogen-enhanced metal-poor (NEMP) stars (Beveridge & Sneden 1994). The cyan and brown shaded regions indicate yields of CCSN (Watanabe et al. 2023) and the equilibrium value of the CNO cycle (Maeder et al. 2015), respectively. The orange dashed line shows a chemical evolution model that reproduces emission-line ratios of quasars (Hamann & Ferland 1993), while nitrogen enrichment in the model is mainly caused by asymptotic giant branch (AGB) stars. The potential change in N/O and C/O due to dust depletion (Ferland et al. 2013) is indicated by the length of the thin black arrow in the bottom left corner of the bottom right panel.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: N III]/O III] (top left), N IV]/O III] (bottom left), C III]/N III] (top right), and C III]/N IV] (bottom right) ratios as a function of N IV]/N III]. Observed emission-line ratios of GLASS_150008, CEERS_01019, and GN-z11 are represented by the double red circle, the red square, and the magenta square, respectively. The emission-line ratios of GN-z11 are measured by Maiolino et al. (2023) and Bunker et al. (2023). The blue and cyan curves show the Cloudy (Ferland et al. 2013) photoionization models with ([N/O], [C/N ]) = (0, 0) based on the stellar and AGN radiation, respectively. The green and yellow curves denote the photoionization models with ([N/O], [C/N ]) = (1, −1) based on the stellar and AGN radiation, respectively. Line styles of these curves (solid, dashed, and dotted) correspond to the assumed metallicities (﹩\mathrm{log}(Z/{Z}_{\odot })=0.25﹩, −0.5, and −1, respectively). Detailed measurements of the N/O and C/N ratios are made in Sections 3.4 and 3.5.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: Comparison with the observed line ratios and the AGN photoionization models with different ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ (top), N/O (middle), C/O (bottom left), and C/N (bottom right). The observed emission-line ratios of CEERS_01019 and GN-z11 are shown by the red and magenta shaded regions, respectively. The black dashed lines in the top panels denote the emission-line ratios predicted by the AGN models with the U values determined by [O III]/[O II] and N IV]/N III] for CEERS_01019 and GN-z11, respectively. The gray shaded regions (in the top panels) represent uncertainties of the observed ionization parameters, while the gray shaded regions in the middle and bottom panels correspond to the uncertainties including both the U and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ uncertainties.
Paper: NuSTAR Hard X-Ray Monitoring of Gravitationally Lensed Quasar RX J1131–1231
Authors: Cora A. DeFrancesco, Xinyu Dai, Mark Mitchell, Abderahmen Zoghbi, Christopher W. Morgan
Figure caption: X-ray luminosity vs. cutoff energy from a selection of quasars (Bertola et al. 2022). The green and blue curves represent the boundary line for runaway pair production presented as a polynomial in Ricci et al. (2018). We assume an X-ray source size of 10r  g . Arrows in place of error bars represent a lower limit on the cutoff energy.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: Emission-line detections of GLASS_150008 and CEERS_01019. (Left) 1″ × 1″ JWST/NIRCam image with blue/green/red corresponding to F150W/F277W/F444W. (Right) Smoothed 1D and 2D spectra around N IV], O III], N III], and C III] shown by the black solid lines and the color maps, respectively. The emission lines are highlighted in yellow, while the highlights for the undetected emission lines are omitted. Rest-frame wavelengths of the emission lines are shown by the vertical black dotted lines. The horizontal gray lines denote the continuum level. The horizontal white lines on the 2D spectra indicate the extraction aperture for the 1D spectra.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: (Left) N IV]/N III] vs. [O III]/[O II] of CEERS_01019 (red square). (Right) [Ne IV]/[Ne III] vs. He II/Hδ of GN-z11 (magenta square). Cloudy photoionization models of young massive stellar population and AGN are shown by the solid and dashed lines, respectively, color coded by metallicity. The observed emission-line ratios are not reproduced by the stellar models but the AGN models are.
Paper: NuSTAR Hard X-Ray Monitoring of Gravitationally Lensed Quasar RX J1131–1231
Authors: Cora A. DeFrancesco, Xinyu Dai, Mark Mitchell, Abderahmen Zoghbi, Christopher W. Morgan
Figure caption: Left: reflection fraction curve. The first point is from the archival XMM-Newton/NuSTAR pair; the rest are paired Swift-NuSTAR observations. Right: change in total, direct, and reprocessed emission over time.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: Metallicity as a function of redshift. The metallicities of CEERS_01019 (red square) and GN-z11 (magenta square) are based on their O/H ratios. The black and blue symbols are FOREVER22 (Yajima et al. 2022, 2023) simulated galaxies of First0 and First1, respectively, while the dots and the solid lines denote metallicities measured within the half-mass radii (r half) and the total gas of the galaxies, respectively.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: Ne/O ratio as a function of ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ (left) and redshift (right). Our sample galaxies, except for CEERS_01019 and GLASS_150008, are the semitransparent red circles. The double circles indicate the measurements with T e determinations. CEERS_01019 is shown by the opaque (AGN assumed) and semitransparent (stellar assumed) red squares, while GLASS_150008 does not have the Ne/O measurement (Table 2). The gray dots in the left panel correspond to the local dwarf galaxies (Izotov et al. 2006; Kojima et al. 2021; Isobe et al. 2022), while the 16th and 84th percentiles of the Ne/O distribution of these local dwarf galaxies are shown by the gray shaded region in the right panel. The blue curves represent chemical evolution models (Watanabe et al. 2023) with different metallicities. The cyan lines denote isochrones of the chemical evolution models at the model ages of 106.7, 106.8, 106.9, and 107.0 yr that correspond to the lifetime of progenitor stars with 40, 30, 25, and 20 M ⊙, respectively (Portinari et al. 1998).