adsabs/AstroCLIMB huggingface dataset:
Paper: reLAISS: A Python Package for Flexible Similarity Searches of Supernovae and Their Host Galaxies
Authors: E. Reynolds, A. Gagliano, V. A. Villar
Figure caption: Top: workflow of the reLAISS library. Starting from user-provided transient coordinates or an optional light curve file, the pipeline (i) identifies the most probable Pan-STARRS host using Prost, (ii) extracts a suite of interpretable light curve and host-galaxy features, (iii) indexes and queries these features with locality-sensitive hashing via ANNOY, and (iv) returns nearest neighbors and highlights anomalies for follow-up. Middle: example nearest neighbor searches. Panel (a) overlays light curves of neighbors for ZTF23aagpjyp, an SN Ia-CSM, identified using light curve features only. Panel (b) charts neighbor host galaxies of the same transient identified using host galaxy features only. Each search used 20 Monte Carlo simulations without PCA. Bottom: example anomaly detection for anomalous transient. Panels (c) and (d) show the light curve of transient ZTF20acpjbgc (a long-duration SN II) and its time-evolving anomaly score.
Paper: Neutral Oxygen in z ∼ 2–3 Galaxies: Probing Galaxy Evolution Through Faint Emission-line Diagnostics
Authors: Audrey Clarendon, Allison Strom, Caroline von Raesfeld
Figure caption: The three classical BPT diagrams for z ∼ 2–3 and z ∼ 0. We plot classification curves from L. J. Kewley et al. (2001, 2006) and G. Kauffmann et al. (2003) to discriminate between ionization mechanisms as well as the z ∼ 2.3 loci from A. L. Strom et al. (2017) on the N2-BPT and S2-BPT. Note that the offset between high (orange and blue points) and low redshift (gray histogram) data is most pronounced on the O1-BPT ((a), (b)) as exemplified by the skew of median log([O III]/Hβ) for bins of log([O I]/Hα) (green stars) away from the maximum starburst diagnostic (red line). CLOUDY-BPASSv2 photoionization models are plotted for Z* = 0.001 and a range of gas-phase enrichment in right column, with darker shading representing higher ionization. Most of the high-redshift data and the median [O I] values fall above model envelopes.
Paper: Identifying Doppelgänger Active Galactic Nuclei Across Redshifts from Spectroscopic Surveys
Authors: Shreya Sareen, Swayamtrupta Panda
Figure caption: Flowchart for an end-to-end pipeline to retrieve doppelgängers across redshift using SDSS DR16 spectroscopic database (Q. Wu & Y. Shen 2022). On the bottom left panels, we are highlighting pairs of AGN spectra for the low-redshift sample and the high-redshift sample. On the extreme right, we highlight one pair of AGN spectra resulting from the analysis for the merged sample. We note that the detection of these doppelgängers is independent of the sky region.
Paper: Determining the Mass and Characteristic Disk Radii of Per-Emb-14 Using Rotation and Infall
Authors: Andrew Milne, Dominique Segura-Cox, Stella Offner
Figure caption: Overlayed position–velocity diagrams for Per-Emb-14. From left to right, the orange contours show the best-fit model for a Keplerian, infalling-rotating envelope, and blended FERIA model. ALMA observations are in blue. Contours were not corrected for radiative transfer effects.
Paper: Crowded Field Photometry with Rubin: Exploring 47 Tucanae with Data Preview 1
Authors: Tobin M. Wainer, James R. A. Davenport, Eric C. Bellm, Yuankun (David) Wang, Neven Caplar, Elliott S. Burdett, Nora Shipp, John K. Parejko, Gray Thoron, Eric Butler, Maya Salwa, Erin Leigh Howard, Brianna Marie Smart, Wilson Beebe, Ishan F. Ghosh-Coutinho, Bob Abel, Željko Ivezić
Figure caption: Top: spatial distributions for 47 Tuc from the DP1 coadd-object catalog (left), and the diaForcedSource median catalog (middle), with both shown for direct comparison (right). Approximate inner completeness radii of ∼28 and ∼14 pc (dashed and dotted lines, respectively) are shown. Bottom: CMDs (left, center) for the coadd-object (left) and diaForcedSource catalogs (middle). Color–color diagram (right) for both samples, with the stellar locus cut described in the text (pink lines).
Paper: lkspacecraft: A Tool for Obtaining Orbital Properties of the Kepler and TESS Spacecraft
Authors: Christina Hedges, Jorge Martínez-Palomera, Amy Tuson, Tyler Pritchard, Rebekah Hounsell, Nicole Schanche, Veselin Kostov, Daniel Giles
Figure caption: Example output of lkspacecraft positions for the full lifetime of the Kepler and TESS missions, shown in 3D coordinates. lkspacecraft enables users to obtain vectors of position, velocity, and light travel time to the solar system barycenter for either spacecraft given an input astropy time. Additionally lkspacecraft enables users to calculate the time of any given observation at the solar system barycenter, the expected velocity aberration of an R.A./decl. coordinate, and the differential velocity aberration of an R.A./decl. coordinate.
Paper: A Preliminary Search for Planets and Exozodiacal Emission Around α Centauri A with JWST/MIRI
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Jorge Llop-Sayson, Laurent Pueyo, Pierre Kervella, Anthony Boccaletti, Pierre-Olivier Lagage, Max Sommer, Mark Wyatt, Nicolas Godoy, Elodie Choquet, Kevin Wagner, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Alexis Bidot, Geoffrey Bryden, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Jarron Leisenring, Jack J. Lissauer, Billy Quarles, Michael Ressler, Eugene Serabyn, Marie Ygouf, Mantas Zilinskas
Figure caption: F1550C image of α Cen AB . α Cen B is saturated near the top and α Cen A is behind the F1550C mask near the center. Two known background stars are labeled (KS2 inset, detected after PSF subtraction; and KS5). The (right) colorbar (for the Stage 2b image) is logarithmically scaled in MJy/sr. A ≈ 3﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 radius region around α Cen A is expanded. (a) The original α Cen AB PSF-subtracted image. Dashed lines indicate the FQPM boundaries. A likely artifact is boxed. (b) An identical reduction after injecting STPSF planet models (circled). (c) An identical reduction after injecting an exozodiacal disk model (boxed). The (bottom) colorbar (for the reduced images and KS2) is linearly scaled in MJy/sr.
Paper: Candidate AGN Extended Emission-line Regions in the Rubin Virgo Field
Authors: Alexander F. Jonkeren, William C. Keel
Figure caption: Montage of gri composite images of EELR candidates from the Rubin first-look Virgo field. Redshifts are spectroscopic (zs) or photometric (zph, averaging Legacy Survey and SDSS estimates). Contrast and saturation have been boosted for candidate E to more clearly show the bluer filament within a tidal tail. North is up and east to the left; angular scales are indicated. Arrows mark the approximate ends of the filament in candidate E.
Paper: The Evolving Light Variations and Periodicities of Betelgeuse Five Years after the Great Dimming
Authors: Jacob Tyler, Ed Marici, Edward Guinan
Figure caption: (a) V-band observations of Betelgeuse from 1995 to 2025; (b) Expanded plot of V-observations after the Great Dimming showing the dominant 208 days period along with the LSP (blue “Xs”); (c) Plot displays the results of the Peranso-3 wavelet WWZ analysis of 1995–2025 data where darker red/orange indicates higher period powers; (d) Peranso-3 wavelet WWZ analysis shows the end of 400 days periodicity and the start of the 208 days periodicity, surprisingly over a year prior to the Great Dimming.
Paper: Determination of the Abundances of the HgMn Star HD 53244 (γ CMa)
Authors: Richard Monier
Figure caption: Left: synthesis of the C II line at 4267.26 Å of HD 53244 (observed spectrum in black, synthetic spectrum in red), Right: synthesis of four Fe II lines from 4500 to 4540 Å.
Paper: Photometric Constraints on Activity of Centaur 174P/Echeclus from 2021 Through 2024
Authors: Aren C. Beck, Charles A. Schambeau, Seamus Walker, Yanga Fernandez
Figure caption: Left: Echeclus’s orbit annotated with its location at known prior outbursts, perihelion, and during our Gemini data collection. Right: radial surface brightness profile of Echeclus compared to a sample of field stars observed on 2022 January 24. The gray shaded region shows the range of scatter of among field star profiles. Inset shows a direct image of Echeclus from the same night.
Paper: Abundance Determinations for HD 32964 A (66 Eri A)
Authors: Richard Monier
Figure caption: Left: synthesis of the Ba II line at 4554.04 Å of 66 Eri A (observed spectrum in black, synthetic spectrum in red), Right: the Y II line at 5662.92 Å is not detected in 66 Eri A but is conspicuous in 66 Eri B.
Paper: Morphology and Stellar Populations of a Candidate Ultra-diffuse Galaxy in Early Euclid and Rubin Imaging
Authors: Aaron J. Romanowsky, Yimeng Tang, Kevin A. Bundy
Figure caption: The candidate UDG SMDG0333094–280938, with Euclid image at top left combining visible (IE) and near-infrared light (YE, HE). The 10″ scale-bar corresponds to 2.7 kpc if the distance is 55 Mpc. The Rubin image is at top middle, combining g, r, i filters. The SED model fit is at lower left, with stellar population results at right, including posteriors on metallicity, mass-weighted age, dust extinction, and cumulative stellar mass.
Paper: Enhancing Multiplet Alignment Measurements with Imaging
Authors: Alexus Annika Kumwembe, Claire Lamman, Daniel Eisenstein, Jessica Nicole Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Andrei Cuceu, Axel de la Macorra, Biprateep Dey, Peter Doel, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Mustapha Ishak, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Ofer Lahav, Martin Landriau, Marc Manera, Ramon Miquel, Seshadri Nadathur, Nathalie Palanque-Delabrouille, Ignasi Pérez-Ràfols, Francisco Prada, Graziano Rossi, Eusebio Sanchez, David Schlegel, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver
Figure caption: The tidal alignment of galaxy multiplets, each containing one spectroscopically measured central galaxy. The gold line is the original measurement made with only spectroscopic data. Although amplitudes vary depending on multiplet definition, their scale-dependent response to large-scale shear is consistent.
Paper: Unexpected Stellar Chemistry as a Marker of Atypical Stellar Evolution?
Authors: Hannah Bohlsen, Amaya Sinha, Gail Zasowski
Figure caption: [Left] [C/N] abundance versus stellar mass for stars in our sample. [Right] Distributions of Neodymium (top) and Europium (bottom) abundances for typical and outlying stars. Neodymium differs strongly between groups, consistent with binary evolution, while Europium is similar and serves as a control since it is not an evolutionary tracer.
Paper: Rapid Dynamical Evolution in the Arjuna Asteroid Belt: Apollo 2022 RD2 Goes from Mini-moon to Virtual Impactor in About 40 yr
Authors: Carlos de la Fuente Marcos, Raúl de la Fuente Marcos
Figure caption: Evolution of the relative mean longitude of 2022 RD2 and its geocentric energy (top), and its geocentric eccentricity and distance (bottom). The origin of time for the top panels is epoch 2461000.5 (2025 November 21.0) TDB and they show the evolution of the nominal orbit (in black) and those of control orbits with state vectors separated ±3σ (light-green/green) and ±9σ (light-/dark-red) from the nominal one. The unit of energy is such that the unit of mass is 1 M⊙, the unit of distance is 1 au, and the unit of time is one sidereal year divided by 2π. The top-right panels focus on the time interval (17.7, 19.0) yr. The bottom-left panel shows the time evolution of the geocentric eccentricity and distance. The bottom-right panel shows the geocentric eccentricity as a function of the geocentric distance. The one Hill radius mark is shown in pink, the three Hill radii mark in red, the capture region in green. The source of the data in the bottom panels is JPL’s Horizons. The output interval is 0.36525 day for the top panels and 5 hr for the bottom panels.
Paper: Mind the Gap in the Extended Kuiper Belt: Statistically Significant Results from New Data
Authors: Carlos de la Fuente Marcos, Raúl de la Fuente Marcos
Figure caption: Heliocentric range and range-rate for the best sample (σr < 1 au, 4188 objects) and statistical significance of the gap. The upper left panel shows the absolute value of the heliocentric range-rate as a function of the range. The upper right panel shows the histogram of heliocentric ranges. The location of the 1:1 mean-motion resonance with Neptune at 30.0 au is shown as a green solid vertical line, the 2:3 resonance at 39.4 au as a blue dashed vertical line, and the 1:2 resonance at 47.8 au as a red dotted–dashed vertical line. The golden vertical line is plotted at 71 au indicating the position of the edge of the gap discussed in the text. In the upper left panel, the two orange dashed vertical lines at 66 and 80 au signal where ﹩| \dot{r}| ﹩ decreases. The bottom panel shows the results of 106 trials of Hartigan’s dip test. Data source: JPL’s Horizons.
Paper: A Simple Procedure for Generating a Kappa Distribution in PIC Simulation
Authors: Seiji Zenitani
Figure caption: (a) Velocity distribution of the Kappa distribution with κ = 2. The black line and the blue histogram show the theoretical curve and numerical results. (b) Acceptance efficiency in the (κ, n) space (Equation (8)). The thin red line, the red dashed line, and the blue dashed line indicate the optimum line, the near-optimum approximation (n = 2κ/3 − 1/5), and our recommendation (n = κ/2), respectively.
Paper: A Bayesian Analysis of Abiogenesis in the Light of Recent Data from K2-18b
Authors: Lorenzo Mercolli
Figure caption: Posterior distributions for λ. Left: two scenarios from D. S. Spiegel & E. L. Turner (2011) (dotted lines) and for M⊕ ∪ MK2-18b with a log-uniform prior (solid line). Right: Earth only scenario from D. Kipping (2025) (dotted line) and for M⊕ ∪ MK2-18b with the Jeffreys prior (solid line).
Paper: Breakthrough Listen Observations of 3I/ATLAS with the Green Bank Telescope at 1–12 GHz
Authors: Ben Jacobson-Bell, Steve Croft, Ellie White, Andrew P. V. Siemion, Matthew Lebofsky, David H. E. MacMahon
Figure caption: Distribution of hits (circles) and events (stars) over frequency and drift rate. The marker size gives the S/N. The gray-shaded regions show ranges not sampled, including narrow notch filter regions in the L and S bands. The color-shaded regions give the range of drift rates expected from Earth’s orbital motion and rotational motion and 3I/ATLAS’s rotation at each of the four observing bands. These regions do not perfectly align between bands due to 3I/ATLAS’s radial acceleration changing during overhead time between observations. No events lie in the expected drift rate regions.
Paper: Radio Constraints Disfavor Little Red Dots as Scaled-down Super-Eddington Quasars
Authors: Carl Audric Guia, Fabio Pacucci
Figure caption: Predicted radio flux densities at 3.0 GHz for LRDs assuming they are scaled-down versions of the super-Eddington quasar RACS J0320-35 at z = 6.13 (L. Ighina et al. 2025). The three colored lines show results for the UV luminosity ratios fUV = 10−3, 10−2, and 10−1 (i.e., for LRDs with UV luminosities 1043, 1044, 1045 erg s−1). The thick dashed–dotted and dashed black curves show the radio fluxes predicted from the jet powers of the super-Eddington GRRMHD models of F. Pacucci & R. Narayan (2024), corresponding to the X-ray-strong (fjet = 0.9) and X-ray-weak (fjet = 0.08) cases, respectively. The purple horizontal band marks the effective 6σ–10σ detection threshold for individual VLASS images, computed from the documented rms sensitivities of 120 μJy. The yellow band marks the 3σ stacking limits derived in K. Perger et al. (2025), which reach ∼1–2 orders of magnitude deeper than individual detections.
Paper: New TESS Secondary Eclipses Confirm Orbital Decay of Kepler-1658b
Authors: Zoutong Shen
Figure caption: Observed minus calculated (O − C) diagram for Kepler-1658b spanning 13 yr of observations. Primary and secondary eclipse times from Kepler (LC and SC), TESS, and WIRC are shown with different colors and symbols. The best-fit orbital decay model (dashed line) yields dP/dt = − 2.20 × 10−5 minutes per orbit and ﹩{Q}_{\star }^{{\prime} }=2.3\times 1{0}^{4}﹩, with BIC =  − 364.3 and ﹩{\chi }_{\nu }^{2}=1.51﹩. The newly detected TESS secondary eclipses (pink points) provide crucial evidence for the system’s orbital decay.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. XVII. HD 49606 (33 Gem)
Authors: Richard Monier
Figure caption: Left: synthesis of the 4500–4560 Å range of one I profile of 33 Gem (observed ESPaDOnS profile of 33 Gem in black, synthetic spectrum in red). Right: synthesis of the Hg II line at 5677.10 Å.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. XIV. HD 172044
Authors: Richard Monier
Figure caption: Left: Comparison of the NARVAL profile of the Hg II line at 3983.93 Å (in black) with the final synthetic spectrum (in black); Right: the same comparison for the Hg II line at 5677.10 Å.
Paper: Correcting the Coordinates for Old Novae V707 Sco and V721 Sco
Authors: Bradley E. Schaefer
Figure caption: Finder charts for V707 Sco (left panel) and V721 Sco (right panel). These Harvard plates have B-band sensitivity, with the charts ﹩20\,\rm{}^{\prime} \rm{}\,﹩ on each side. The nova in eruption is indicated with the horizontal and vertical tic marks, while the old catalog positions are indicated with the  ×  marks.
Paper: A Quantification Method for Plasma Exchange Across the Planetary Magnetopause Layer
Authors: Zhongwei Yang, Can Huang, Riku Jarvinen, Xiaocheng Guo, Chi Wang
Figure caption: (a) Number density of solar wind ions nsw (cm−3) on the Z = 0 plane; (b) corresponding number density of magnetospheric ions nms (cm−3); (c) mixing rate (mr) calculated from the two ion populations; (d) three-dimensional magnetopause surface delineated by the mixing rate, with color indicating the x-component of the local surface normal unit vector ﹩\hat{{\boldsymbol{n}}}﹩; (e) finite-element triangulated surface of the magnetopause, colored by the area of each surface element dS (﹩{R}_{{\rm{E}}}^{2}﹩); (f) normal component of the particle flux density across the surface, computed as the product of ion bulk velocity and number density ﹩n{\boldsymbol{V}}\cdot \hat{{\boldsymbol{n}}}﹩ (km s−1 · cm−3). Blue and red represent entering and escaping ions, respectively.
Paper: MESA-QUEST: Modeling Quasi-stars in MESA
Authors: Claire B. Campbell, Andrew D. Santarelli, Matthew E. Caplan
Figure caption: MESA and Ball (2011) Comparison: (Top) Density as a function of radial profile (left) and outer and Bondi radius as a function of black hole mass (right) from W. H. Ball et al. (2011) (dashed) and our fiducial MESA model (solid) using (ϵ,  η) = (0.1,  0.1). For the density, these profiles are chosen to match available data from W. H. Ball et al. (2011) and are not evenly spaced in time. (Bottom) Surface (left) and core (right) properties of our quasi-star as functions of black hole mass, including model ages.
Paper: Analysis of Trajectories to 3I/ATLAS with a Comet Interceptor-like Spacecraft
Authors: Joan Pau Sanchez, Colin Snodgrass
Figure caption: Top-down view of the inner solar system showing the spacecraft trajectory (green) intercepting 3I’s path (purple), in a reference frame rotating with the Earth. The red box shows the location of the deep space manoeuvre (DSM) in the middle of the cruise. Dates are DD/MM/YYYY format.
Paper: Radially Extended C I Emission in the IM Lup Protoplanetary Disk Uncovered with Matched Filtering
Authors: Thomas Maher, Charles J. Law, L. Ilsedore Cleeves
Figure caption: Top: [C I] 1–0 channel map of the IM Lup disk with a representative annular Keplerian mask (dashed lines) with Rmax = 4﹩\mathop{.}\limits^{{\prime\prime} }﹩5, i.e., for an annulus between a radius of 4﹩\mathop{.}\limits^{{\prime\prime} }﹩0 and 4﹩\mathop{.}\limits^{{\prime\prime} }﹩5. The LSRK velocity and synthesized beam are shown in the upper right and bottom left corner, respectively, of each panel. Bottom: peak filter response as a function of outer mask radius for binary (left) and power-law (right) pixel values. The dashed red line marks the radial extent of C I in the image plane (C. J. Law et al. 2023).
Paper: One Million Open-source Cislunar Orbits
Authors: Travis Yeager, Denvir Higgins, Peter McGill, Kerianne Pruett, Alexx Perloff, Tara Grice, Michael Schneider
Figure caption: Sample orbit of an L4-bound lunar Trojan, demonstrating six years of stability. Color represents time progression, starting with purple and transitioning through the rainbow toward red. The blue dot at the center marks the Earth’s position over time. In this reference frame, the Moon is fixed at (0, 0, 0); due to the Moon’s orbital eccentricity, the Earth appears to move slightly over time.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XXI. HD 53588
Authors: Richard Monier
Figure caption: Left: synthesis of the 4500–4560 Å spectral interval (observed spectrum in black, synthetic spectrum in red), Right: TESS lightcurve of HD 53588.
Paper: Characterization of the Visual Binary TOI-6883AB and its Dynamical Implications for the Planetary Companion TOI-6883Ab
Authors: Giuseppe Conzo, Fran Campos, Francesco Conti, Ian Sharp
Figure caption: Ground-based light curve of TOI-6883Ab obtained on 2024 August 21 from Spain at Observatori Puig Agulles using RC 14″ f/8 on EQ8; SBIG ST-8XME and Johnson–Cousins Ic filter (on top) and from UK at PixelSkies using Celestron C11 F/7; SX 694 TRIUS PRO and Johnson–Cousins Rc filter (on bottom). Timing offset of ∼1.0 hr is the same.
Paper: Roche-lobe Overflow Ejecta Cannot Explain Carbon Enhancement of GDR3-0928
Authors: Zhongyuan Zhang, Alexander P. Ji
Figure caption: (a) Shaded “CEMP-formation region” in wind-velocity–density space for an accretion time of 104 yr. The three regions correspond to α = 0.1, 0.3, 0.7, where αM0 is the minimum carbon-rich mass that a star with mass M0 must accrete to show CEMP abundances. (b) Outflow parcels from RLOF simulation of M. Y. M. Lau et al. (2022). There are points with R ≈ 100 au in the blue region corresponding to t = 104 yr. (c) Grid produced from analytic model of W. Lu et al. (2022). Points intersecting with the blue region require unphysical ﹩\dot{{M}_{1}}\approx 0.1{M}_{\odot }﹩ yr−1. (d) Maximum mass Macc the remote star can accrete before a 12M⊙ donor star is depleted, as a function of ﹩\dot{{M}_{1}}﹩ and binary separation a in astronomical unit. Values remain at least seven orders of magnitude below the CEMP-forming threshold.
Paper: Dinner with a Star: Stellar Engulfment of Exoplanet Systems
Authors: Ashlyn R. Leary, M. Virginia McSwain
Figure caption: This figure depicts the evolutionary tracks produced by MESA for various stellar masses, beginning at the ZAMS and ending at 3α ignition. The planets predicted to be swallowed by their host star are plotted as gray dots at the evolutionary position of the host star when R = a.
Paper: The Sonora Substellar Atmosphere Models. V. A Correction to the Disequilibrium Abundance of CO2 for Sonora Elf Owl
Authors: Nicholas F. Wogan, James Mang, Natasha E. Batalha, Kevin Zahnle, Sagnick Mukherjee, Channon Visscher, Jonathan J. Fortney, Mark S. Marley, Caroline V. Morley
Figure caption: CO2 (left) and CO (center) quenching in a brown dwarf atmosphere with Teff = 500 K, a 31 m s−2 gravity, 0.1× solar metallicity, solar carbon-to-oxygen, and a vertically constant Kzz = 108 cm2 s−1. The green dashed lines are the results of a full kinetics simulation using the Photochem code. CO (right) quenches with respect to the full atmosphere equilibrium (blue dotted line). CO2 (left) quenches with respect to the already quenched abundances of CO (black dotted line). The Sonora Elf Owl v1 published in S. Mukherjee et al. (2024) quenched CO2 with respect to the full atmosphere equilibrium, under predicting the gases abundance by two order of magnitude (black solid line, left panel). The right panel compares the emission spectra of Elf Owl v1 (with the CO2 under-predicted) and Elf Owl v2 (with the CO2 corrected) for this substellar atmosphere.