adsabs/AstroCLIMB huggingface dataset:
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: Left: image of centaur 39P obtained with the 4.3 m LDT using the ﹩{r}^{{\prime} }﹩ filter on 2022 September 18 UTC. 39P is at the center of the image, marked with two lines. This image was obtained 57 days after the JWST data but provides useful context. The image scale and orientation with respect to the J2000 equatorial reference frame are shown, as well as the projected centaur–Sun vector (⊙ = 64°) and the projected velocity vector (v = 68°). Right: 2× zoomed image of 39P taken with the LDT.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: The production rates per unit area of 39P compared against other centaurs and comets are shown. This CO2/D2 plot is an updated version of Figure 12 from Harrington Pinto et al. (2022). 39P shows a low production rate per unit area, like the upper limit for 29P from Ootsubo et al. (2012).
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: Left: Gemini-North telescope image of centaur 39P obtained using the ﹩{r}^{{\prime} }﹩ filter on 2022 July 28 UTC. 39P is at the center of the image, marked with two white lines. The image scale and orientation with the J2000 equatorial reference frame are shown, as well as the projected comet–Sun vector (⊙ = 68°) and the projected velocity vector (v = 68°). Right: 2× zoomed image of 39P taken with Gemini-North.
Paper: Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
Authors: David Polishook, Francesca E. DeMeo, Brian J. Burt, Cristina A. Thomas, Andrew S. Rivkin, Juan A. Sanchez, Vishnu Reddy
Figure caption: Spectral slope measured by IRTF (colored squares; same color scheme as in Figures 4 and 7) compared to the changing brightness of the Didymos system (in absolute magnitude values in the V band, usually marked as H  v ) following the impact as measured by the Danish 1.54 m telescope (black circles; Rożek et al. 2023). The linear slopes of the two parameter sets were drawn at the same scale using a coefficient of 10.27 and a constant of 16.04 (black and orange dashed lines). The photometry of the Danish telescope was used for its 1.″5 aperture, which is the most equivalent to the IRTF/SpeX 0.″8 slit width. The photometric error (∼0.04 mag) is smaller than the size of the symbols. The transparent background represents the decreasing contribution of the ejecta from Dimorphos to the overall light. The transparency value used (written as a percentage at the bottom of each section) is the ratio calculated from the Danish telescope photometry. The uncertainty of these ratios is ∼5%. Before the impact, Dimorphos's surface is about 5% of Didymos's surface.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: The sampling of the cone axes in the 15° radius uncertainty region around R.A., decl.: 136°,+5°. For each axis, we have computed the best solution that fits LUKE observation IDs 2-7. Each axis therefore has a combination of R.A., decl., η, γ, and ω that defines their best score in fitting the data. The lower the score, the better the reproduction of LUKE observations. Axes with best scores lower than 6° are represented as circles, whereas axes with best scores greater than 6° are represented as crosses. The filled circles correspond to axes with solutions that are compatible with the observation ID 1, while empty circles correspond to solutions that do not agree with the observation ID 1. The solutions corresponding to the filled circles are listed in Table A1.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Each panel corresponds to a LUKE observation where the ejecta cone is observed projected in a side-on profile or a similar geometry. The corresponding timestamps are given in the panel titles. The first panel explores all cones with an elliptical base in the selected restricted η and γ space, and their scores are given in the scatter plot. The following panels show how the scores evolve for a given cone, as constraints are placed by different LUKE observations. The panels should be followed from left to right and top to bottom. Thus, the last panel isolates the viable solutions of η and γ that best describe the LUKE observations. The contrasting very high scores correspond to η and γ combinations that are discontinued from the iterations as they do not fall within the imposed cone edge orientation constraints.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Three orthogonal views of the intersection of the ejecta cone and the surface of the Dimorphos, leading to the definition of the perimeter of the crater created by the DART impact. The sphere with a radius of 10 m shows the location of the DART impact. The orange dot marks the center of Dimorphos.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Simulations of LUKE observation IDs 1-8 using the axis solution of R.A., decl.: 147°,+16° using a cone with an elliptical base defined by η = 69°, γ = 51°, and ω = 12°. The top panel corresponds to IDs 1 through 4, and the bottom panel corresponds to IDs 5 through 8.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: The scores shown in different panels of Figure 6 are averaged here and are represented in a narrower scale than in Figure 6 in order to highlight the viable solutions of η and γ.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Simulations of LUKE observation IDs 1-8 using the axis solution of R.A., decl.: 136°,+5° using a cone with an elliptical base defined by η = 64°, γ = 39°. The top panel corresponds to IDs 1 through 4, and the bottom panel corresponds to IDs 5 through 8.
Paper: Characterization of the DART Impact Ejecta Plume on Dimorphos from LICIACube Observations
Authors: J. D. P. Deshapriya, P. H. Hasselmann, I. Gai, M. Hirabayashi, E. Dotto, A. Rossi, A. Zinzi, V. Della Corte, I. Bertini, S. Ieva, E. Mazzotta Epifani, M. Dall'Ora, S. Ivanovski, D. Perna, T. L. Farnham, M. Amoroso, J. R. Brucato, A. Capannolo, S. Caporali, M. Ceresoli, Nancy L. Chabot, A. Cheng, G. Cremonese, R. T. Daly, E. G. Fahnestock, L. Gomez Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, J.-Y. Li, M. Lombardo, A. Lucchetti, D. Modenini, M. Pajola, E. Palmer, P. Palumbo, S. Pirrotta, G. Poggiali, A. S. Rivkin, P. Sanchez, G. Tancredi, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Geometry of LICIACube observations that were used to derive the location of the cone apex.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Transit transmission spectra (at 1 cm−1 resolution, R = 10,000 at 1 μm) of modern (preindustrial) Earth-like TRAPPIST-1 e environments, and similar environments with increased fluxes of CH3Cl. Strong features from CO2 and CH4 are seen, as well as weaker features from O2, O3, and N2O. Increased CH3Cl influences atmospheric chemistry by reducing the abundance of other biosignatures such as CH4 and O3, and it produces strong CH3Cl spectral features only at fluxes orders of magnitude stronger than modern Earth. An additional (gray) line for Rayleigh scattering and refraction only is also shown. For TRAPPIST-1 e refraction has a negligible contribution (the transit height is less than 1 km), and Rayleigh scattering influences transit spectra predominantly in the visible.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Transit transmission spectra (at 1 cm−1 resolution, R = 10,000 at 1 μm) of TRAPPIST-1 e Archean-like and enhanced sulfur organics environments. CH4 and CO2 produce some of the more detectable features, as well as hydrocarbon haze, which contributes substantially to the higher transit continuum at less than 3.2 μm and at 5.5–6.2 μm. There are also numerous hydrocarbon absorbers between 2–4 μm and 5–14 μm—not all contributing gases are labeled. In hazy atmospheres, the haze and organic molecules combine to form a strong pseudocontinuum from 8–15 μm.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Transmission spectrum model (at 1 cm−1 resolution) of TRAPPIST-1 e assuming that it possesses a 1 bar sulfur organic biosphere with a thick hydrocarbon haze. The simulated data are shown with error bars corresponding to 50 transits with NIRSpec Prism (top panel) and 100 transits with MIRI LRS (bottom panel), both binned to a resolving power of ﹩{ \mathcal R }=20﹩. Individual absorption features are shaded in color to indicate the molecule responsible for the absorption. Despite the presence of numerous biosignature gases in the mid-IR with strong features (e.g., DMS, C2H6, and CH3SH), CO2, CH4, and organic haze are the most detectable potential biosignatures for these environments.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Comparison of the transmission spectrum (at 1 cm−1 resolution, R = 10,000 at 1 μm) for simulations of TRAPPIST-1 e with a preindustrial oxygenic Earth-like atmosphere (dark blue, 452 ppm CH4) and a methanogenic, Archean-Earth-like atmosphere (orange line, 253 ppm CH4), both with 5% CO2. The environments produce similar CH4 features, but modern Earth has O2/O3 features and the Archean produces sufficient C2H6 for a weak band at 12 μm. This result suggests that the CH4 and CO2 bands from methanogenesis can be a persistent feature throughout a planet’s history.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Transmission spectrum (at 1 cm−1 resolution, R = 10,000 at 1 μm) for the modern (preindustrial) Earth-like TRAPPIST-1 d. The high cloud deck truncates features throughout the spectrum, particularly the Chappuis band of ozone. The warmer and higher-altitude cold trap and subsequent higher stratospheric water vapor abundance produce additional visible-region water features and obscure the available CO2 bands, except the strongest at 4.3 and 15 μm. The methane features are relatively weak owing to photochemical destruction via water photolysis and truncation of the absorption features by the formation of very high altitude water clouds. There is no Rayleigh scattering slope owing to the high-altitude cloud tops.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Theoretical transmission spectrum (at 1 cm−1 resolution) of TRAPPIST-1 d with a cloudy modern-Earth-like atmosphere. The shaded color regions show the contribution of the dominant absorbing molecules to the spectrum. Simulated data points and error bars are shown for 30 transits (binned to a resolving power of ﹩{ \mathcal R }=20﹩) with NIRSpec Prism (NGROUP = 6), which is sufficient for ﹩\left\langle {\rm{S}}/{\rm{N}}\right\rangle \approx 5﹩ on H2O and ﹩\left\langle {\rm{S}}/{\rm{N}}\right\rangle \approx 3﹩ on CO2. For reference, the NIRSpec spectrograph with the double-pass low-resolution prism has a spectral resolving power R (λ/Δλ) of 30–300, and that with the high-resolution G140H grating has an R of 1300–2300 (Jakobsen et al. 2022).
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Comparison of the transmission spectrum (at 1 cm−1 resolution, R = 10,000 at 1 μm) for TRAPPIST-1 e for methanogenic, Archean Earth (orange line), with 5% CO2, and a prebiotic Earth (dark green) with enhanced volcanic outgassing and 1.9% CO2. Both environments exhibit strong CO2 features, with the biogenic environment producing stronger CH4 features. The prebiotic Earth is more easily distinguished by its large CO band at 4.6 μm.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Comparison of the transmission spectrum (at 1 cm−1 resolution, R = 10,000 at 1 μm) for TRAPPIST-1 e with the temperature and gas abundance profiles of the true Earth (cloudy Earth orbiting a G dwarf; cyan line), which is not photochemically self-consistent with the spectrum of TRAPPIST-1, vs. the cloudy preindustrial Earth case, which is photochemically self-consistent with the spectrum of TRAPPIST-1 and has similar clouds (dark-blue line). For the same surface flux, the self-consistent preindustrial Earth produces much stronger CH4 features owing to higher atmospheric abundances under favorable chemistry driven by the TRAPPIST-1 stellar spectrum. The CO2 features for our self-consistent Earth are larger only as a result of requiring a higher abundance to remain temperate.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Simulated data and transmission spectrum model (at 1 cm−1 resolution) of TRAPPIST-1 e assuming that it possesses a 1 bar Archean-Earth-like atmosphere with a methanogenic biosphere (warm Archean Earth case). The spectrum is shown with water clouds in the atmosphere, with error bars calculated for 15 transits observed with JWST/NIRSpec Prism (binned to a resolving power of ﹩{ \mathcal R }=20﹩). The shaded color regions show the contribution of the dominant absorbing molecules to the spectrum, which notably shows large and detectable CO2 and CH4 features and small and undetectable H2O and CO features.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: TRAPPIST-1 e modeled photochemical equilibrium species profiles for inhabited Archean and a prebiotic Earth-like atmosphere with enhanced volcanism (line types), for oxygen-bearing compounds (left panel), hydrocarbons (middle panel), and sulfur-bearing compounds (right panel). The Archean warm planet and the prebiotic planet both have water clouds, and the Archean cold planet has both water clouds and a photochemically generated hydrocarbon haze. The prebiotic planet does not contain a biosphere and shows the atmospheric abundances expected for vigorous outgassing from a more reducing mantle. Note that the warm Archean CO2 and prebiotic atmosphere CO overlap at approximately 5% abundance in the left panel.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: TRAPPIST-1 e modeled photochemical equilibrium species profiles for cloudy modern-Earth-like atmospheres with nominal and enhanced CH3Cl surface fluxes. The modern-Earth-like clear-sky case is not shown here but is similar to the nominal (cloudy) case. The left panel shows all climatically or spectrally relevant species except CH3Cl and HCl, which are shown in the right panel, along with key radical Cl. True Earth vertical profiles for H2O, O3, and CH4 (thick lines in the left panel) are shown for comparison.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: Calculated aerosol differential optical depth (optical depth per kilometer of altitude) profiles for our modeled TRAPPIST-1 d and e environments. The aerosol optical properties used and the calculation of cloud-layer optical depths and altitudes are described in Section 2.4.3. The TRAPPIST-1 d Earth-like environment is warmer than the true Earth (modern Earth orbiting the Sun), and its condensation water clouds form at higher altitudes. The cold Archean climate is modeled with higher, more distributed ice clouds, due to the much colder temperatures, and has a smaller total optical depth, due to reduced overall condensation. Except for the cold Archean and the additional haze optical depths, cumulative cloud optical depths are τ = 2.25.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: TRAPPIST-1 e modeled photochemical equilibrium species profiles for sulfur-enhanced Archean-Earth-like atmospheres, for oxygen-bearing compounds (left panel), hydrocarbons (middle panel), and sulfur-bearing compounds (right panel). Four different Archean-Earth-like atmospheres with enhanced sulfur fluxes are plotted in each panel (line types) for dominant methanogenic and sulfur biospheres and with clouds or hazes.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: TRAPPIST-1 e modeled climates, with the true Earth’s (modern Earth orbiting the Sun) climate for comparison (black line). Many cases exhibit a secondary cold trap at 100–300 Pa. However, the cases with enhanced sulfur fluxes and low CO2 exhibit haze absorption heating, which results in a long adiabat, high cold trap, and mild stratosphere. In addition, the greenhouse heating of hydrocarbon and reduced sulfur gases in the atmosphere counter the anti-greenhouse of the haze to the extent that Earth-like levels of CO2 maintain a temperate surface. Although increasing Cl levels also decrease CH4 abundance, those planets generate lower stratospheric H2O, with a net cooling of the stratospheres and heating of the surface. The altitude scale for Earth is provided for rough comparison.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: TRAPPIST-1 d temperature (black line) and modeled photochemical equilibrium species profiles for the cloudy modern preindustrial Earth-like atmosphere. Due to the higher atmospheric temperature and lower gravity of TRAPPIST-1 d, the atmosphere is significantly extended in the vertical direction, with a stratosphere spanning 80–140 km. Water is also nearly evenly mixed throughout the vertical column.
Paper: The Feasibility of Detecting Biosignatures in the TRAPPIST-1 Planetary System with JWST
Authors: Victoria S. Meadows, Andrew P. Lincowski, Jacob Lustig-Yaeger
Figure caption: UV spectra comparison, for the Sun (black), average of calibrated models from Peacock et al. (2019; gray), and the same model with spurious UV lines removed (red; S. Peacock, personal communication).