adsabs/AstroCLIMB huggingface dataset:
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption: Comparison between reductions and systematics treatments. (a) Comparison between the (combined) transmission spectra resulting from the three reduction pipelines. Solid and semitransparent points are from spectral orders 1 and 2, respectively. Horizontal dashed lines show the error-weighted average transit depths. (b) Comparison between the transit spectra of visit 2 resulting from the five different systematics treatments. In both panels, the number in parentheses in the legends is the median error bar across each spectrum. All vertical error bars are 1σ uncertainties. All horizontal error bars represent the extent of each spectral bin.
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption: Signatures of stellar variability and activity between and within the two visits. (a) Median extracted spectrum of visits 1 (blue) and 2 (orange), zoomed in on the 1.24–1.25 μm K I doublet. Uncertainties are smaller than the line width. Shaded regions show the two different definitions of the continuum adopted to compute the EW of the reddest of the two lines of the doublet. (b) Median quiescent (out-of-flare) stellar spectrum of visit 2 (blue) and stellar spectrum at maximum Hα luminosity (orange), i.e., at the peak of the flare in visit 2. Error bars are 1σ uncertainties.
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption: NIRISS/SOSS broadband (white) and spectrophotometric (colored) transit light curves. Panels (a)–(c) correspond to visit 1 and (d)–(f) to visit 2. All error bars are 1σ uncertainties. (a) and (d) Light curves. (b) and (e) Light-curve residuals from the best-fit model. (c) and (f) Distribution of the light-curve residuals, with a Gaussian distribution overplotted for comparison.
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption:  POSEIDON posterior distribution for visit 2. This corresponds to the simultaneous fit of the stellar contamination and planetary atmosphere for the second TRAPPIST-1 b transit (see Section 5.2).
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption:  POSEIDON posterior distribution for visit 1. This corresponds to the simultaneous fit of the stellar contamination and planetary atmosphere for the first TRAPPIST-1 b transit (see Section 5.2).
Paper: Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn
Authors: Guochao Sun, Claude-André Faucher-Giguère, Christopher C. Hayward, Xuejian Shen, Andrew Wetzel, Rachel K. Cochrane
Figure caption: Top: UV magnitude–halo mass relations at z = 8–12. Data for individual galaxies are denoted by the gray dots (no smoothing applied to the SFH). The thick solid curves indicate the range of the 5th and 95th percentiles in the “bursty” and “smoothed” cases, from which the suppression of bright galaxy number counts due to smoothing is apparent. Bottom: UVLFs at z = 8–12 derived from the convolution between the UV magnitude–halo mass relation and the HMF. Dust-free predictions are shown as solid for both “bursty” and “smoothed” cases, whereas the dust-attenuated scenario is shown as dashed for only the “bursty” case (Section 2.2.2) for visual clarity. Constraints from observations are shown by the data points in black for the spectroscopically confirmed-only samples (Harikane et al. 2023a) and in gray for data sets involving photometric candidates (Oesch et al. 2018; Bowler et al. 2020; Rojas-Ruiz et al. 2020; Bouwens et al. 2021, 2023; Finkelstein et al. 2022; Leethochawalit et al. 2023; Castellano et al. 2023; Donnan et al. 2023; Harikane et al. 2023a; Pérez-González et al. 2023). Cases with larger and smaller smoothing timescale τ SF values than the fiducial one (100 Myr) are shown at z = 10 to illustrate the impact of SFH smoothing on the UVLF.
Paper: Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn
Authors: Guochao Sun, Claude-André Faucher-Giguère, Christopher C. Hayward, Xuejian Shen, Andrew Wetzel, Rachel K. Cochrane
Figure caption: Dust-free UVLFs at z = 8, 10, and 12 predicted by the FIRE-2 simulations and from the literature. The binned and the best-fit, double-power law UVLFs are denoted by the crosses and solid curves, as specified in Table 1 and Equation (1), respectively. Several example dust-free predictions from other cosmological hydrodynamical simulations, including MillenniumTNG (dashed; Kannan et al. 2023), FLARES (dotted; Vijayan et al. 2021; Wilkins et al. 2023), and CoDa II (dotted and only at z = 8 and 10; Ocvirk et al. 2020; Dawoodbhoy et al. 2023) are also plotted for comparison.
Paper: Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn
Authors: Guochao Sun, Claude-André Faucher-Giguère, Christopher C. Hayward, Xuejian Shen, Andrew Wetzel, Rachel K. Cochrane
Figure caption: The cumulative UV luminosity density ﹩{\rho }_{\mathrm{UV}}(\lt {M}_{\mathrm{UV},\mathrm{lim}})﹩ integrated down to ﹩{M}_{\mathrm{UV},\mathrm{lim}}\simeq -18﹩ with dust attenuation included (see Section 2.2.2). At z ≳ 10, some theoretical models (e.g., Mason et al. 2015; Harikane et al. 2018) underestimate ρ UV compared with observational constraints based on photometric galaxy candidates (e.g., Bouwens et al. 2023; Donnan et al. 2023; McLeod et al. 2023; Pérez-González et al. 2023) and/or spectroscopically confirmed galaxies as firm lower limits (Harikane et al. 2023a). Predictions from our “bursty” case are broadly consistent with both photometric and spectroscopic samples and show a slightly weaker redshift evolution ρ UV ∝ (1 + z)−0.3 over 8 ≤ z ≤ 12.
Paper: Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn
Authors: Guochao Sun, Claude-André Faucher-Giguère, Christopher C. Hayward, Xuejian Shen, Andrew Wetzel, Rachel K. Cochrane
Figure caption: The number of galaxies sampled in each halo mass bin for the 26 simulations inspected for evaluating the UVLF at z = 10 ± 0.5. This amounts to a total of ≈9000 galaxies sampled from snapshots of the 26 zoom-in regions over 9.5 < z < 10.5. Simulation IDs are listed in the legend (see Sun et al. 2023a).
Paper: On the Magnetic Nature of Quiet-Sun Chromospheric Grains
Authors: María Jesús Martínez González, Tanausú del Pino Alemán, Adur Pastor Yabar, C. Quintero Noda, Andrés Asensio Ramos
Figure caption: Panel (a) represents the cumulative functions of the amplitude of Stokes V/I divided by the noise level (7 × 10−4) for those pixels that harbor calcium grains. Dotted lines display the values of the original data, while solid lines are the result of averaging each individual patch. In all panels, blue lines correspond to the Fe I data, and orange ones to the Ca II data. Panels (b), (c), and (d) display the histograms for the Stokes V/I amplitude, continuum intensity (Fe I) or wing intensity (Ca II), and intensity line depth. Solid lines are the pixels with calcium grains while dotted lines are the rest of the pixels. Panel (e) displays the map of Stokes V/I amplitude at the photosphere. The contours encircle those pixels with calcium grains, as obtained with the k-means algorithm. The yellow circles in panel (e) mark the positions of the three examples shown in the work. The topmost circle marks the position of the example shown in Figure 3, the middle one marks the example displayed in Figure 4, and the bottom one marks the position of the example found in Figure 5. Panel (f) displays the initial time at which the calcium grains appear.
Paper: On the Magnetic Nature of Quiet-Sun Chromospheric Grains
Authors: María Jesús Martínez González, Tanausú del Pino Alemán, Adur Pastor Yabar, C. Quintero Noda, Andrés Asensio Ramos
Figure caption: Time evolution of a region centered at [6, 49] arcsec in the FOV. The background image in the top panel represents the intensity at Δλ = −0.21 Å, where the emission-like feature of the grain appears. The values of the intensity range between 0.2 I  c  and 0.6 I  c . The background in the second panel from the top displays the absolute value of the average Stokes V amplitude in three pixels centered at Δλ = −0.21 Å. The background image in the third panel from the top is the absolute value of the amplitude of Stokes V of the full profile of the Ca II line. The background image in the bottom panel is the absolute value of the Stokes V amplitude of the Fe I line. The salmon contours in all panels contain Stokes V amplitudes of the Fe I line larger than or equal to 3 × 10−3 I  c . More details on its computation can be found in the text. The values of the Stokes V amplitudes of both the Ca II and the Fe I lines range from zero to 2 × 10−3 I  c . The yellow dots mark the positions of the profiles drawn in Figure 3.
Paper: On the Magnetic Nature of Quiet-Sun Chromospheric Grains
Authors: María Jesús Martínez González, Tanausú del Pino Alemán, Adur Pastor Yabar, C. Quintero Noda, Andrés Asensio Ramos
Figure caption: Time evolution of the Stokes I (upper inset) and Stokes V (bottom inset) for the pixels marked with yellow dots in the top panel of Figure 1.
Paper: On the Magnetic Nature of Quiet-Sun Chromospheric Grains
Authors: María Jesús Martínez González, Tanausú del Pino Alemán, Adur Pastor Yabar, C. Quintero Noda, Andrés Asensio Ramos
Figure caption: Time evolution of the Stokes I (upper inset) and Stokes V (bottom inset) for a pixel centered at the bottom yellow circle in panel (e) of Figure 2.
Paper: On the Magnetic Nature of Quiet-Sun Chromospheric Grains
Authors: María Jesús Martínez González, Tanausú del Pino Alemán, Adur Pastor Yabar, C. Quintero Noda, Andrés Asensio Ramos
Figure caption: Time evolution of the Stokes I (upper inset) and Stokes V (bottom inset) for a pixel centered at the middle yellow circle in panel (e) of Figure 2.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: HARPS RVs of GJ 367 phase-folded at the orbital period of the USP planet and best-fitting model as derived using the FCO method. The different colors refer to the 96 different nightly chunks, which include at least two measurements per night.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: Results of a Bayesian analysis of the internal structure of GJ 367 b. The depicted internal structure parameters are as follows: the mass fractions of the inner iron core and a possible water layer with respect to the solid planet without a possible H/He layer), the molar fractions of Si and Mg within the silicate mantle layer, the molar fraction of iron in the inner core, the logarithm with base 10 of the mass of the H/He layer in Earth masses, and the shift in the Fe/Si ratio of the planet with respect to the Fe/Si ratio in the host star, again in a logarithmic scale. The titles in each column show the median of the posterior distributions and the 5th and 95th percentiles.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: Mass–radius diagram of small USP planets (P < 1 days, R < 2 R ⊕, M < 10 M ⊕) with masses and radii known with a precision better than 20%, as retrieved from the Transiting Extrasolar Planet Catalogue (Southworth 2011). From bottom to top, the solid and dashed curves are theoretical models from Zeng et al. (2016). We highlighted GJ 367 b with a red dot and the previous position on the diagram with a black dot (Lam et al. 2021).
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: RV and differential line width (DLW) time series with best-fitting models from the multi-GP (solid black lines) and the 1σ and 2σ credible intervals of the corresponding GP models (light gray shaded areas). The upper panel shows the RV data with the full model in black, while the planetary signal (blue), and stellar (red) inferred models are shown with a vertical offset for clarity. The lower panel shows the DLW along with the stellar inferred model. Data are shown with filled circles, with their nominal error bars and semitransparent error bar extensions accounting for the inferred jitter term.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: HARPS RV time series of GJ 367 along with the best-fitting five-signal model (three planets + stellar rotation + long-period stellar signal). Data are shown as blue filled circles with their nominal uncertainties. The vertical gray lines mark the error bars including the RV jitter.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: Phase-folded RV curves of GJ 367 b (a), GJ 367 c (b), GJ 367 d (c), stellar rotation (d), and long-period stellar signal (e). Data are shown as blue filled circles with their nominal uncertainties. The vertical gray lines mark the error bars including the RV jitter.
Paper: Company for the Ultra-high Density, Ultra-short Period Sub-Earth GJ 367 b: Discovery of Two Additional Low-mass Planets at 11.5 and 34 Days 
Authors: Elisa Goffo, Davide Gandolfi, Jo Ann Egger, Alexander J. Mustill, Simon H. Albrecht, Teruyuki Hirano, Oleg Kochukhov, Nicola Astudillo-Defru, Oscar Barragan, Luisa M. Serrano, Artie P. Hatzes, Yann Alibert, Eike Guenther, Fei Dai, Kristine W. F. Lam, Szilárd Csizmadia, Alexis M. S. Smith, Luca Fossati, Rafael Luque, Florian Rodler, Mark L. Winther, Jakob L. Rørsted, Javier Alarcon, Xavier Bonfils, William D. Cochran, Hans J. Deeg, Jon M. Jenkins, Judith Korth, John H. Livingston, Annabella Meech, Felipe Murgas, Jaume Orell-Miquel, Hannah L. M. Osborne, Enric Palle, Carina M. Persson, Seth Redfield, George R. Ricker, Sara Seager, Roland Vanderspek, Vincent Van Eylen, Joshua N. Winn
Figure caption: Phase-folded RVs curve of GJ 367 b (a), GJ 367 c (b), and GJ 367 d (c). Data are shown as filled green circles with the error bars and the light-green error bars accounting for the inferred RV jitter term.
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption: NIRISS/SOSS transit spectra of TRAPPIST-1 b compared to stellar-contamination and atmosphere models from the sequential analysis. Black circles are the SOSS transit spectra, either from visit 1 (a), visit 2 (b), or from both visits combined ((c)–(d)). In panels (c) and (d), the transit spectra are corrected from stellar contamination. Dashed lines are the error-weighted mean transit depths. Vertical error bars are 1σ uncertainties. Horizontal error bars represent the extent of each spectral bin. (a)–(b) Comparison between the transmission spectrum of each visit to its best-fit/median stellar-contamination model (black/orange curves) and uncertainties (shaded regions). (c) Gray, thin error bars are the SOSS transit depths at higher spectral resolution. Blue points are the Hubble Space Telescope (HST)/WFC3 and Spitzer/IRAC transit depths (de Wit et al. 2016, 2018; Zhang et al. 2018; Ducrot et al. 2020a), vertically shifted to match the median of the SOSS data. Clear, hydrogen-rich models in orange and green can be ruled out at 29 and 16σ, respectively. (d) Clear 100% CH4 (red), CO2 (green), H2O (orange), and Titan-like (purple) atmospheres cannot be rejected or confirmed.