adsabs/AstroCLIMB huggingface dataset:
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: The left and right panels show the variation in the [Fe II] 1.533 μm/1.644 μm and [S II] 1.0286 μm/1.0336 μm flux ratios with the electron density, respectively. The solid curves correspond to an electron temperature of 10,000 K and the dashed–dotted curves to 20,000 K. The dashed colored lines show ratios of the total observed fluxes for all sources, as listed in Table 3. The [Fe II] curves were created using atomic data and collision strengths from S. S. Tayal & O. Zatsarinny (2018). Similarly, the [S II] curves were made using atomic data from P. Rynkun et al. (2019) and collision strengths from S. S. Tayal & O. Zatsarinny (2010), using PyNeb (V. Luridiana et al. 2015).
Paper: Asymmetry and Dynamical Constraints in Two-limbs Retrieval of WASP-39 b Inferring from JWST Data
Authors: Zixin Chen, Jianghui Ji, Guo Chen, Fei Yan, Xianyu Tan
Figure caption: Comparison of retrieved results: cloud-top pressure (﹩\mathrm{log}{P}_{{\rm{c}}}﹩[bar]), Rayleigh-like scattering slope (γ), and logarithmic scattering enhancement factor (﹩\mathrm{log}A﹩) across JWST full, JWST cutoff, and Pre-JWST data sets. Results are shown for valmorn (blue) and valeven (red), under fixed (dark) and free (light) models. Error bars represent uncertainties for each parameter.
Paper: Asymmetry and Dynamical Constraints in Two-limbs Retrieval of WASP-39 b Inferring from JWST Data
Authors: Zixin Chen, Jianghui Ji, Guo Chen, Fei Yan, Xianyu Tan
Figure caption: The retrieved transmission spectra for four 2D atmospheric models (2D Fixed Model A, 2D Fixed Model B, 2D Free Model A, and 2D Free Model B) derived from JWST NIRSpec/PRISM observations. Each panel represents the results for one of the models, divided into four subplots illustrating: (1) the total observed transit depth; (2) the normalized residuals; (3) the limb-specific (morning and evening) contributions to the transmission spectrum; and (4) the difference between morning and evening limb depths ΔD.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Each subplot shows the jet mass-loss rate estimates as a function of the distance from the source using three different methods. In blue is method 1 (Section 5.2.1), in orange is method 2 (Section 5.2.2), and in green is method 3 (Section 5.2.3). The error bars represent 30% uncertainty for HH 30 and FS TauB and 50% for Tau 042021 and IRAS 04302, as described in the text.
Paper: Asymmetry and Dynamical Constraints in Two-limbs Retrieval of WASP-39 b Inferring from JWST Data
Authors: Zixin Chen, Jianghui Ji, Guo Chen, Fei Yan, Xianyu Tan
Figure caption: The retrieved results of composition parameters of three data sets and four models. The C/O upper limit of 0.7 is reported by (Z. Rustamkulov et al. 2023) through the full JWST NIRSpec/PRISM observation.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Each subplot shows the shock regions in the blue- and redshifted jet lobes, identified in the extinction-corrected [Fe II] intensity (log) profile plotted as a function of the distance from the star. Gray dashed–dotted lines highlight the local minima used to locate the shock regions.
Paper: Asymmetry and Dynamical Constraints in Two-limbs Retrieval of WASP-39 b Inferring from JWST Data
Authors: Zixin Chen, Jianghui Ji, Guo Chen, Fei Yan, Xianyu Tan
Figure caption: Temperature mapping from shallow-water simulation of WASP-39 b.
Paper: Asymmetry and Dynamical Constraints in Two-limbs Retrieval of WASP-39 b Inferring from JWST Data
Authors: Zixin Chen, Jianghui Ji, Guo Chen, Fei Yan, Xianyu Tan
Figure caption: Supplement to Figure 2. Retrieved limb-specific spectra for four 2D atmospheric models derived from JWST NIRSpec/PRISM observations, with wavelengths less than 2 μm removed. This allows a direct comparison with the observational limb spectra reported by N. Espinoza et al. (2024).
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: (Left) APF spectra of the directly imaged companion host star 51 Eri (cyan) around the C I line at 5052 Å. Overplotted are PHOENIX-C/O models at the best-fit T eff and ﹩\mathrm{log}g﹩ of 51 Eri, but carbon abundances ranging from −0.2 dex (blue, dotted) to solar (magenta, dashed–dotted) to +0.2 dex (green, dashed). The oxygen abundance is kept constant at solar values for all models. The PHOENIX-C/O model is a good fit for our data, and this grid can resolve the differences in flux due to varying carbon abundance. (Right) Same as the figure on the left, but for varying oxygen abundances around the O I triplet at 6155–58 Å. The carbon is kept constant at solar abundance for all models. While the models seem to have offsets from the science spectra in certain wavelength pockets (e.g., 6147–51 Å), these offsets do not coincide with carbon and oxygen lines of interest and are consistent across different carbon and oxygen abundances, Hence, they are probably due to an issue in the models that does not impact the carbon and/or oxygen abundances.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Best-fit PHOENIX-C/O model of the APF spectrum for the target 51 Eri (cyan), shown for order #87 containing a blended C I line at 5380 Å. Some significant spectral absorption lines in this order have been labeled. The zoomed-in subplot on the right shows a ∼10 Å region around the blended line, with the lines considered in the C I blend marked individually. The best-fit PHOENIX-C/O model has T eff = 7277 K, ﹩\mathrm{log}g﹩ = 4.32, ﹩\mathrm{log}{\epsilon }_{{\rm{C}}}﹩ = 8.46, and ﹩\mathrm{log}{\epsilon }_{{\rm{O}}}﹩ = 8.73 (magenta). The residuals between the data and the model are plotted in black, and other noise limits are shown in gray. While the model fit is excellent around the blended C I line, it does not fit well around some of the other lines, probably due to the use of the solar-metallicity PHOENIX-C/O grid and/or other unknown systematics in the stellar atmospheric models. Due to these irregularities between the model and the spectra, we fit for only a small region around the spectral line of interest while determining carbon and oxygen abundances.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Continuum-normalized spectra of the host star 51 Eri (blue) illustrating the procedure for measurement of the equivalent width of the oxygen triplet feature at 6155–58 Å. We fit two independent Gaussian profiles (orange dashed and green dashed–dotted lines) to the blended feature and adjust the parameters of the two Gaussians such that the sum of the two profiles (purple dashed line) fits the observed spectral feature. Subsequently, trapezoidal integration on the area under the Gaussian blend gives the equivalent width of the blended feature. The black dotted line at the bottom shows the continuum level.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Best-fit PHOENIX model of the APF spectrum for the target 51 Eri (cyan), shown for APF order #74. The broader absorption features correspond to stellar features, while the sharper ones (those similar to spikes) correspond to telluric features. The parameters of the best-fit PHOENIX model are estimated by computing the median for the effective temperature (T eff), surface gravity (﹩\mathrm{log}g﹩), and the metallicity ([M/H]) over nine retained runs after performing multiple multi-order MCMC runs. This model has T eff = 7277 K, ﹩\mathrm{log}g﹩ = 4.32, [M/H] = −0.01 (magenta). The residuals between the data and the model are plotted in black, and other noise limits are shown in gray.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for a multi-order fit of the PHOENIX grid to the spectrum of 51 Eri. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run gives a best-fit T eff = 7215 K, ﹩\mathrm{log}g﹩ = 4.27, and [M/H] = −0.01.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Walker plot from an MCMC run for the determination of stellar atmospheric parameters for the host star 51 Eri. The MCMC was run with 100 walkers for 1750 steps, with the first 1250 discarded as burn-in. Convergence was achieved in this run, as seen by the behavior of the walkers, which begin to converge to a definite value around step ∼1200 for all parameters. The corner plot corresponding to this run is shown in Figure 5.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for the PHOENIX-C/O grid fit to the spectrum of 51 Eri. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run gives a best-fit ﹩\mathrm{log}{\epsilon }_{{\rm{C}}}﹩ = 8.43, ﹩\mathrm{log}{\epsilon }_{{\rm{O}}}﹩ = 8.79.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Abundances relative to solar for the 15 elements with abundances measured using the equivalent-width method. The black dotted line denotes where the abundance of an element is solar. Relative abundances are shown for all five targets in this paper. We note that HR 8799 has consistently subsolar abundances (except C and O), while GJ 504 has consistently supersolar average abundances (except Mg). For the other three host stars, the abundances of most elements are solar with no consistent trend regarding which element(s) deviate(s) from solar. Overall, we do not notice any unusual abundance patterns among the stars that host directly imaged planets that persist for the whole sample.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Companion C/O ratio relative to the stellar C/O ratio plotted against the companion mass in M Jup. Most companions effectively have stellar C/O ratios at the 1σ level. Only GJ 504 b has a nonstellar (substellar) C/O ratio; however, the C/O ratio of this companion is highly model-dependent and hence still uncertain. Stellar C/O ratios are from Table 4 and planetary parameters are from Table 6. We assume a mass of 2–4M Jup for 51 Eri b (S. B. Brown-Sevilla et al. 2023) and a C/O = ﹩{0.82}_{-0.19}^{+0.04}﹩ for HD 206893 B from J. Kammerer et al. (2021).
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Best-fit PHOENIX model of the APF spectrum for the target HD 984 (cyan), shown for APF order #79. The parameters of the best-fit PHOENIX model are estimated by computing the median for the effective temperature (T eff), surface gravity (﹩\mathrm{log}g﹩), and metallicity ([M/H]) over seven retained runs after performing multiple multi-order MCMC runs. This model has T eff = 6401 K, ﹩\mathrm{log}g﹩ = 4.42, and [M/H] = −0.01 (magenta). The residuals between the data and the model are plotted in black, and other noise limits are shown in gray.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Best-fit PHOENIX model of the APF spectrum for the target HR 8799 (cyan), shown for APF order #72. The parameters of the best-fit PHOENIX model are estimated by computing the median for the effective temperature (T eff), surface gravity (﹩\mathrm{log}g﹩), and metallicity ([M/H]) over seven retained runs after performing multiple multi-order MCMC runs. This model has T eff = 7317 K, ﹩\mathrm{log}g﹩ = 4.32, and [M/H] = −0.57 (magenta). The residuals between the data and the model are plotted in black, and other noise limits are shown in gray.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Best-fit PHOENIX model of the APF spectrum for the target GJ 504 (cyan), shown for APF order #78. The parameters of the best-fit PHOENIX model are estimated by computing the median for the effective temperature (T eff), surface gravity (﹩\mathrm{log}g﹩), and metallicity ([M/H]) over seven retained runs after performing multiple multi-order MCMC runs. This model has T eff = 5959 K, ﹩\mathrm{log}g﹩ = 4.65, and [M/H] = 0.12 (magenta). The residuals between the data and the model are plotted in black, and other noise limits are shown in gray.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Best-fit PHOENIX model of the APF spectrum for the target HD 206893 (cyan), shown for APF order #82. The parameters of the best-fit PHOENIX model are estimated by computing the median for the effective temperature (T eff), surface gravity (﹩\mathrm{log}g﹩), and metallicity ([M/H]) over 10 retained runs after performing multiple multi-order MCMC runs. This model has T eff = 6617 K, ﹩\mathrm{log}g﹩ = 4.27, and [M/H] = 0.06 (magenta). The residuals between the data and the model are plotted in black, and other noise limits are shown in gray.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for a multi-order fit of the PHOENIX grid to the spectrum of HR 8799. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run gives a best-fit T eff = 7490 K, ﹩\mathrm{log}g﹩ = 4.32, and [M/H] = −0.50.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for a multi-order fit of the PHOENIX grid to the spectrum of HD 984. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run gives a best-fit T eff = 6332 K, ﹩\mathrm{log}g﹩ = 4.59, and [M/H] = −0.03.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for a multi-order fit of the PHOENIX grid to the spectrum of GJ 504. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run gives a best-fit T eff = 6072 K, ﹩\mathrm{log}g﹩ = 4.80, and [M/H] = 0.13.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for the PHOENIX-C/O grid fit to the spectrum of HD 206893. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run is one of those performed with the carbon abundance fixed to 8.57 ± 0.03 (obtained in the carbon-only runs performed beforehand). We obtain a best-fit ﹩\mathrm{log}{\epsilon }_{{\rm{C}}}﹩ = 8.56, ﹩\mathrm{log}{\epsilon }_{{\rm{O}}}﹩ = 8.65 from this MCMC run.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for the PHOENIX-C/O grid fit to the spectrum of HR 8799. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run is one of those performed with the carbon abundance fixed to 8.56 ± 0.04 (obtained in the carbon-only runs performed beforehand). We obtain a best-fit ﹩\mathrm{log}{\epsilon }_{{\rm{C}}}﹩ = 8.56, ﹩\mathrm{log}{\epsilon }_{{\rm{O}}}﹩ = 8.80 from this MCMC run.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Corner plot for one of the retained runs for the PHOENIX-C/O grid fit to the spectrum of GJ 504. The marginalized posteriors are shown along the diagonal. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The subsequent covariances between all the parameters are in the corresponding 2D histograms. This run is one of those performed with the carbon abundance fixed to 8.70 ± 0.03 (obtained in the carbon-only runs performed beforehand). We obtain a best-fit ﹩\mathrm{log}{\epsilon }_{{\rm{C}}}﹩ = 8.68, ﹩\mathrm{log}{\epsilon }_{{\rm{O}}}﹩ = 8.97 from this MCMC run.
Paper: A High-resolution Spectroscopic Survey of Directly Imaged Companion Hosts. I. Determination of Diagnostic Stellar Abundances for Planet Formation and Composition
Authors: Aneesh Baburaj, Quinn M. Konopacky, Christopher A. Theissen, Sarah Peacock, Lori Huseby, Benjamin J. Fulton, Roman Gerasimov, Travis S. Barman, Kielan K. W. Hoch
Figure caption: Best-fit PHOENIX-C/O model of the APF spectrum for the target GJ 504 (cyan), shown for order #76 containing an O I triplet feature at 6155–6158 Å. The zoomed-in subplot on the right shows a ∼10 Å region around the slightly blended feature. The best-fit PHOENIX-C/O model has T eff = 5959 K, ﹩\mathrm{log}g﹩ = 4.65, ﹩\mathrm{log}{\epsilon }_{{\rm{C}}}﹩ = 8.70, and ﹩\mathrm{log}{\epsilon }_{{\rm{O}}}﹩ = 8.97 (magenta). The residuals between the data and the model are plotted in black, and other noise limits are shown in gray.