adsabs/AstroCLIMB huggingface dataset:
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Molecular gas mass vs. SFR. As background contours, we show literature star-forming samples: COLDGASS detected (gray), undetected (red; A. Saintonge et al. 2011), and PHIBSS/PHIBSS2 (blue; L. J. Tacconi et al. 2018; J. Freundlich et al. 2019). As green diamonds, we show literature post-starburst samples (S. Belli et al. 2021; C. Woodrum et al. 2022; P.-F. Wu et al. 2023), with SFRs derived from SED fitting that incorporates MIR data. In black, we show SQuIGG﹩\overrightarrow{L}﹩E, with the SFRs measured in K. A. Suess et al. (2022a). Under the assumptions in that fitting (and with αCO = 4.0), the entire SQuIGG﹩\overrightarrow{L}﹩E  sample lies below the SFR–﹩{M}_{{{\rm{H}}}_{2}}﹩ relation, suggesting that star formation in SQuIGG﹩\overrightarrow{L}﹩E  post-starburst galaxies at fixed ﹩{M}_{{{\rm{H}}}_{2}}﹩ is low relative to typical star-forming galaxies.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: As in Figure 2, but showing only the HSC image, the CO(2–1) Moment 0 map, and the collapsed CO(2–1) spectrum for the entire rest of the new galaxies (sorted by CO(2–1) luminosity) presented in this work.
Paper: Removing Atmospheric Turbulence from Ground-based Astrometry with Fast Correlation Function Measurements
Authors: Daniel C. H. Gomes, Gary M. Bernstein, Claire-Alice Hébert
Figure caption: The turbulence variance reduction factor (﹩{C}_{0}^{\rm{pre}\,}/{C}_{0}^{\,\rm{post}}﹩) is plotted as a function of the reference star density on LSST simulations (black) and real DES exposures (purple). The solid black shows the median variance reduction attained for LSST simulations with a fixed 1 mas measurement uncertainty per star. The gray zone represents 1σ exposure-to-exposure rms variation. The simulations shown with black dashed line also include expected magnitude-dependent LSST measurement noise per star, with higher density values representing the use of fainter-than-Gaia reference stars. The black dotted line is a power-law fit to the variance reduction in the noiseless scenario. The magenta dots are individual DES exposures; the solid line, their median value, and the dotted line, a power-law fit.
Paper: Disequilibrium Chemistry, Diabatic Thermal Structure, and Clouds in the Atmosphere of COCONUTS-2b
Authors: Zhoujian Zhang, 周健 张, Sagnick Mukherjee, Michael C. Liu, Jonathan J. Fortney, Emily Mader, William M. J. Best, Trent J. Dupuy, Sandy K. Leggett, Theodora Karalidi, Michael R. Line, Mark S. Marley, Caroline V. Morley, Mark W. Phillips, Robert J. Siverd, Joseph A. Zalesky
Figure caption: Masses (top) or mass ratios (bottom) of confirmed exoplanets (collected from the NASA Exoplanet Archive on 2024 June 21) as functions of their orbital separations (gray), with those having observed transmission and emission spectra highlighted in orange and blue, respectively. Substellar binaries with dynamical masses are shown in green (T. J. Dupuy et al. 2016; T. J. Dupuy & M. C. Liu 2017; P. F. Lazorenko & J. Sahlmann 2018; T. J. Dupuy et al. 2019; G. Chabrier et al. 2023; T. J. Dupuy et al. 2023). Solar system planets are plotted with sizes unscaled. Brown-dashed lines highlight the planet mass of 13 M Jup and the planet-to-host mass ratio of 0.04, as adopted by the IAU working definition of exoplanets.
Paper: Disequilibrium Chemistry, Diabatic Thermal Structure, and Clouds in the Atmosphere of COCONUTS-2b
Authors: Zhoujian Zhang, 周健 张, Sagnick Mukherjee, Michael C. Liu, Jonathan J. Fortney, Emily Mader, William M. J. Best, Trent J. Dupuy, Sandy K. Leggett, Theodora Karalidi, Michael R. Line, Mark S. Marley, Caroline V. Morley, Mark W. Phillips, Robert J. Siverd, Joseph A. Zalesky
Figure caption: Top panel: The 1–25 μm SED of COCONUTS-2b, including our new Gemini/F2 spectrum (blue) and the WISE (green) and Spitzer (purple) photometry. This object’s W1 and W2 photometry are from CatWISE, with proper motion accounted for; the W4 photometry is an upper limit. The spectral flux uncertainties are shown as light shades. Bottom panel: The Gemini/F2 spectrum with key spectral features labeled. Fluxes in gray shades are masked for the subsequent forward-modeling analysis in Section 4.
Paper: Disequilibrium Chemistry, Diabatic Thermal Structure, and Clouds in the Atmosphere of COCONUTS-2b
Authors: Zhoujian Zhang, 周健 张, Sagnick Mukherjee, Michael C. Liu, Jonathan J. Fortney, Emily Mader, William M. J. Best, Trent J. Dupuy, Sandy K. Leggett, Theodora Karalidi, Michael R. Line, Mark S. Marley, Caroline V. Morley, Mark W. Phillips, Robert J. Siverd, Joseph A. Zalesky
Figure caption: Forward-modeling results based on models with disequilibrium chemistry, diabatic temperature–pressure (T–P) profiles, and no clouds. For each grid, the observed spectrophotometry of COCONUTS-2b (blue) and the maximum-likelihood model spectrum (orange) are plotted in the top panel; the best-fit T eff, ﹩\mathrm{log}(g)﹩, and [M/H] values are labeled. The gray-shaded regions indicate the masked wavelengths in the forward-modeling analysis. The bottom panel shows the data−model residuals, with the significance values labeled for the broadband photometry. The unit of plotted fluxes is 10−17 erg s−1 cm−2 Å−1. The ΔBIC of a given grid is computed relative to the BIC of the PH  3  -free ATMO2020++ results.
Paper: Disequilibrium Chemistry, Diabatic Thermal Structure, and Clouds in the Atmosphere of COCONUTS-2b
Authors: Zhoujian Zhang, 周健 张, Sagnick Mukherjee, Michael C. Liu, Jonathan J. Fortney, Emily Mader, William M. J. Best, Trent J. Dupuy, Sandy K. Leggett, Theodora Karalidi, Michael R. Line, Mark S. Marley, Caroline V. Morley, Mark W. Phillips, Robert J. Siverd, Joseph A. Zalesky
Figure caption: Top panel: Reduced χ 2 values of the fitted T0–Y1 spectral templates. The best-matched template with the lowest ﹩{\chi }_{\nu }^{2}﹩ has a T9.5 spectral type. Bottom panel: The Gemini/F2 spectrum of COCONUTS-2b (blue; with downgraded spectral resolution) overlaid with five best-fitted spectral templates (black). The masked wavelength ranges in this comparison are highlighted in gray shades, which are different from the gray shades shown in Figure 2.
Paper: CRIRES+ and ESPRESSO Reveal an Atmosphere Enriched in Volatiles Relative to Refractories on the Ultrahot Jupiter WASP-121b
Authors: Stefan Pelletier, Björn Benneke, Yayaati Chachan, Luc Bazinet, Romain Allart, H. Jens Hoeijmakers, Alexis Lavail, Bibiana Prinoth, Louis-Philippe Coulombe, Joshua D. Lothringer, Vivien Parmentier, Peter Smith, Nicholas Borsato, Brian Thorsbro
Figure caption: Retrieved temperature structure and abundance profiles on the dayside atmosphere of WASP-121b. The results from the hybrid-free retrieval considering parameterized H2O dissociation are shown in blue while the chemical equilibrium retrieval results are shown in green. Left panel: inferred vertical temperature-pressure profile of WASP-121b (68% and 95% confidence interval contours) compared to a one-dimensional radiative-convective equilibrium PHOENIX model (J. D. Lothringer et al. 2020; pink solid line), a three-dimensional GCM (V. Parmentier et al. 2018; yellow solid line), and previous results using the Hubble Space Telescope (T. Mikal-Evans et al. 2022; black contour, 1σ credible range at the pressures probed by the data). Right panels: Retrieved abundance profiles for H2O, CO, Fe, Ni, H−, and e− (in order from top left to bottom right). In the hybrid-free retrieval, abundance profiles are assumed to be uniform-in-pressure except for H2O and H−, which are fitted using the parameterization of V. Parmentier et al. (2018) to take into account thermal dissociation. Here, we see that, for H2O in particular, dissociation is important at pressures below ∼10 millibar. Meanwhile, we find that, for our retrieved temperature structure of WASP-121b, the chemical equilibrium abundance profile predicted for CO and Fe can still be reasonably well approximated as being constant with altitude. This is in contrast to Ni, which ionizes more readily compared to Fe and for these temperatures is expected to appear underabundant at submillibar pressures. With its greater flexibility, uncertainties are generally larger for the hybrid-free retrieval, in particular for parameters for which we have little sensitivity to, such as the abundance of free electron. Overall, we find that the dayside atmosphere of WASP-121b has a strong thermal inversion and that our abundance estimates from both retrieval approaches are compatible.
Paper: CRIRES+ and ESPRESSO Reveal an Atmosphere Enriched in Volatiles Relative to Refractories on the Ultrahot Jupiter WASP-121b
Authors: Stefan Pelletier, Björn Benneke, Yayaati Chachan, Luc Bazinet, Romain Allart, H. Jens Hoeijmakers, Alexis Lavail, Bibiana Prinoth, Louis-Philippe Coulombe, Joshua D. Lothringer, Vivien Parmentier, Peter Smith, Nicholas Borsato, Brian Thorsbro
Figure caption: Retrieved elemental composition of the dayside atmosphere of WASP-121b from both the free (blue) and chemical equilibrium (green) retrievals. Shown in the panel from left to right are the marginalized probability constraints for the inferred abundance of refractories, abundance of volatiles, ratio of volatiles to refractories, and C/O ratio in the atmosphere of WASP-121b. Values for the Sun (orange) and host star (red) are also depicted for comparison. While the abundance of refractories on WASP-121b is marginally elevated but consistent with previous works (S. Gandhi et al. 2023; C. Maguire et al. 2023) and the stellar value to about 1σ, the abundance of volatiles is slightly superstellar, more consistent with a Jupiter-like degree of enrichment (∼4× solar, black dashed line). Combined, the volatile-to-refractory ratio is elevated with respect to both solar and stellar values, suggesting that WASP-121b has an atmosphere that is enriched in ices relative to rocks. The retrieved high C/O ratio, especially in comparison with the host star, also potentially indicates that WASP-121b may have accreted its envelope in a carbon-rich environment. Overall, both the free and chemical equilibrium retrievals find relatively consistent results, with the volatile and refractory abundances as well as the volatile-to-refractory and carbon-to-oxygen ratios on WASP-121b all being enriched relative to both the Sun and WASP-121 (the host star).
Paper: CRIRES+ and ESPRESSO Reveal an Atmosphere Enriched in Volatiles Relative to Refractories on the Ultrahot Jupiter WASP-121b
Authors: Stefan Pelletier, Björn Benneke, Yayaati Chachan, Luc Bazinet, Romain Allart, H. Jens Hoeijmakers, Alexis Lavail, Bibiana Prinoth, Louis-Philippe Coulombe, Joshua D. Lothringer, Vivien Parmentier, Peter Smith, Nicholas Borsato, Brian Thorsbro
Figure caption: Measured elemental abundance ratios on WASP-121b compared to predictions from different formation scenarios. Here, each colored dashed line corresponds to a predicted elemental composition for the considered giant planet formation scenarios (see Y. Chachan et al. 2023; and Section 5), compared to the retrieved values for WASP-121b (black and gray contours, 39.3%, 86.5%, and 98.9% confidence intervals). All abundance ratios are normalized to the stellar value (dotted gray lines). Left panel: O/Fe and C/Fe comparison, where the greater enrichment in C compared to O relative to Fe is consistent with formation scenarios beyond the H2O snowline or near the CO snowline (scenarios 5, 6, and 7). Right panel: Fe/H and C/Fe comparison now showing all scenarios except those enriched by CO gas or solids (scenarios 6 and 7, light and dark blue lines) being ruled out by the measured stellar-like refractory abundance. Under this model, the only formation scenarios consistent with the measured refractory and volatile abundances is if WASP-121b accreted its envelope in a volatile-rich, high C/O environment near the CO snowline.
Paper: CRIRES+ and ESPRESSO Reveal an Atmosphere Enriched in Volatiles Relative to Refractories on the Ultrahot Jupiter WASP-121b
Authors: Stefan Pelletier, Björn Benneke, Yayaati Chachan, Luc Bazinet, Romain Allart, H. Jens Hoeijmakers, Alexis Lavail, Bibiana Prinoth, Louis-Philippe Coulombe, Joshua D. Lothringer, Vivien Parmentier, Peter Smith, Nicholas Borsato, Brian Thorsbro
Figure caption: Abundance enrichment for elements on WASP-121b compared to the solar system giants. Here, the planetary atmosphere enrichment levels are measured relative to host star (gray dashed line) abundances, namely, WASP-121 (A. S. Polanski et al. 2022) for WASP-121b or the Sun (M. Asplund et al. 2021) otherwise. C abundances for the solar system giants are inferred from CH4 measurements (see S. K. Atreya et al. 2020 and references therein) while the O abundance for Jupiter is from Juno (C. Li et al. 2024). No Fe or Ni measurements exist for Jupiter, Saturn, Uranus, or Neptune to compare to due to their cold temperatures causing all rock-forming elements to be condensed out of the upper atmosphere. While here all planets show enhanced metallicities relative to their host star for volatile elements (particularly C), WASP-121b does not show such an elevated enrichment for refractory elements.
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: Left: the Keck-HIRES RV time series from A. S. Polanski et al. (2024). Data are shown with an arbitrary offset such that the first observation is plotted at Time = 0. RVs are binned in units of 0.1 days. Right: histogram of the time differences between consecutive RVs. Note the intranight cadence for TOI-1444, which hosts a USP planet.
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: The mass–radius diagram in the sub-Neptune and super-Earth regime. Contours are computed using Gaussian kernel density estimation on the population of confirmed planets with better than 33% and 15% measurement precision on mass and radius, respectively (NASA Exoplanet Archive 2024). Composition curves are shown for reference. The two dashed–dotted light blue curves represent Earth-like cores surrounded by 1% and 2% by mass H-/He-dominated, solar-metallicity envelopes for a planet receiving 10 times Earth’s insolation orbiting a 10 Gyr-old star (E. D. Lopez & J. J. Fortney 2014). HD 119130 b’s instellation is S p = 67 S ⊕. The solid red, green, and brown curves represent a pure iron, Earth-like, and pure silicate composition, respectively (L. Zeng et al. 2016). The dashed dark blue curve represents an irradiated “water world” at T eq = 800 K made of an Earth-like core and 50% H2O, by mass, in the form of a supercritical H2O fluid layer and a steam-dominated envelope; the solid dark blue curve represents a composition of 100% supercritical H2O and steam at T eq = 800 K (A. Aguichine et al. 2021). HD 119130 b is shown as both the square (L19 mass measurement) and the star (this work) for comparison.
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: The results of the resampling experiment for HD 119130 b following the methods of J. M. Akana Murphy et al. (2024). Each cell represents a resampled realization of the full data set according to specified MOC (left y-axis; i.e., a lower limit enforced on the time between consecutive measurements) and N RV (x-axis) values. The right y-axis is the same as the left, but it is now shown in units of the orbital period of the planet. The color of each cell represents the difference between the planet’s measured semiamplitude using that cell’s resampled data set, K fit, and the measured semiamplitude of the planet from the baseline model (K baseline), in units of the uncertainty on K baseline. Gray regions represent combinations of MOC and N RV that are not supported by the data. The rightmost non-gray cell along the bottom row represents the original time series and is therefore in agreement with K baseline by construction.
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: Top: GLS periodogram of a synthetic RV time series generated by assuming the L19 orbital solution for HD 119130 b and producing an RV at each observation time stamp in our real data set. We assume typical measurement errors and white noise. The vertical blue line marks the orbital period of HD 119130 b. As before, the horizontal lines correspond to the 10%, 1%, and 0.1% FAP thresholds. If the planet did indeed have K b = 6 m s−1, it would have been easily detected in our data, assuming it is the only periodic signal present. Bottom: the residuals of the synthetic RVs after removing the L19 orbit for planet b.
Paper: HD 119130 b Is Not an “Ultradense” Sub-Neptune
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha, Ilaria Carleo, Enric Palle, Madison Brady, Benjamin Fulton, Luke B. Handley, Howard Isaacson, Gaia Lacedelli, Felipe Murgas, Grzegorz Nowak, J. Orell-Miquel, Hannah L. M. Osborne, Vincent Van Eylen, María Rosa Zapatero Osorio
Figure caption: A map of best-fitting K 1 values fit using a one-planet model but where the (synthetic) data contain a second signal at P 2 = 12 days. The second signal is specified by the different combinations of K 2 and ϕ 2. We see that in certain cases, K 1 is inflated to values similar to the result from L19.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Instellation flux as a function of planet escape velocity, in log–log scale. Based on data from the NASA Exoplanet Archive (2024) downloaded on 2024 June 30. The empirical “cosmic shoreline” and the water vapor greenhouse runaway threshold (K. J. Zahnle & D. C. Catling 2017) are shown as cyan and yellow shaded regions, respectively. Planets are categorized into terrestrial planets (magenta), sub-Neptunes (blue), Neptune-like planets (green), and gas giants (yellow) based on radius, see legend. The red rectangles represent escape velocities calculated based on HD 101581 planets’ mean estimated masses assuming Hypatia Catalog metallicity. Because only radius, but not mass, is known, we further plot light red regions covering all possible interior compositions, ranging from pure iron to pure silicates. The heights of the rectangles represent uncertainties in insolation.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Estimated TSM and ESM values (E. M. R. Kempton et al. 2018) for known terrestrial planets (R  p  < 1.5 R ⊕) with TSM > 10, based on their properties given in the NASA Exoplanet Archive Planetary Systems Composite Data Table (NASA Exoplanet Archive 2024). Planets are colored by equilibrium temperature assuming zero albedo. Sub-Earths (R  p  < 1 R ⊕) are plotted with a black outline. The top right-hand box indicates the TSM/ESM parameter space in which the planets lie. The planets orbiting HD 101581are among the best sub-Earths for characterization with both transmission and emission spectroscopy.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Expected transmission spectra for all three planets, assuming a CO2-dominated, Venus-like atmosphere (black) or O2-dominated atmosphere (gray) at 10 bar surface pressure. Simulated JWST/NIRCam long wavelength grism observations of the CO2-dominated atmosphere using the SUBGRISM64 array (useful for extremely bright hosts) is shown for the F322W2 filter (blue) and F444W filter (orange). The JWST data have been rebinned to R = 20 and assume only one transit per planet. At TSM = 37.3, 32.8, and 30.4, all three planets are among the top six sub-Earth-size planets for transmission spectroscopy.