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: NIRISS/SOSS broadband light-curve fits, Hα integrated flux, and spectral trace morphology metrics. Panels (a)–(h) correspond to visit 1 and panels (i)–(p) to visit 2. All error bars are 1σ uncertainties. (a) & (i) Observed light curve (black points) and best-fit model (blue curve). (b) & (j) Light-curve residuals from the best-fit model. (c) & (k) Histogram of the light-curve residuals normalized by the scatter (bars) and a Gaussian distribution (blue curve) for comparison. (d) & (l) Time series of the integrated flux of the Hα stellar line. (e) & (m) Amplitude of the trace displacement in the spectral direction (b(t) in text). (f) & (n) Amplitude of the trace displacement in the cross-dispersion direction (c(t)). (g) & (o) Amplitude of the trace rotation (d(t)). (h) & (p) Amplitude of the second derivative of the trace profile in the cross-dispersion direction (e(t)). For visit 2, the shaded blue domain highlights the stellar flare. The jump in the broadband flux (j) and in the Hα integrated flux (l) are not linked to any anomaly in the spectral trace morphology ((m)–(p)).
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: Atmospheric and stellar properties from the transmission spectra of TRAPPIST-1 b from the simultaneous stellar-contamination and planetary atmosphere fit. (a)–(b) Retrieved model spectrum of TRAPPIST-1 b from two retrievals: a stellar-contamination model with unocculted spots and faculae (orange) and a joint stellar-contamination and planetary atmosphere model (purple), for visits 1 and 2. The median retrieved model (solid lines) and the corresponding 1σ and 2σ confidence intervals (dark and light contours, respectively) are compared to the observed TRAPPIST-1 b spectrum (black points). Error bars are 1σ uncertainties. (c)–(d) Corresponding posterior probability distributions from the joint stellar-contamination and planetary atmosphere retrieval for visits 1 and 2. The TRAPPIST-1 b spectra are well fitted by the stellar-contamination model (﹩{\chi }_{\nu }^{2}﹩= 1.07 and 0.75 for the best-fitting model spectra to visits 1 and 2, respectively), with no fit improvement from adding a thick planetary atmosphere. However, the CO2 and H2O posteriors indicate that a high-mean-molecular-mass atmosphere remains consistent with the TRAPPIST-1 b observations.
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: Joint constraints on the H2/He abundance and the atmospheric pressure on TRAPPIST-1 b resulting from the sequential fit of the stellar contamination and planetary atmosphere. The color shading illustrates the posterior probability density, where darker colors correspond to higher probabilities. Contours indicate the 1σ, 2σ, and 3σ Bayesian credible regions. The displayed posterior probability is marginalized over the H2O, CH4, CO, CO2, NH3, and N2 abundances. Hydrogen-dominated scenarios with high-altitude clouds are at the top left corner of the plot and cloud-free, volatile-rich, high-mean-molecular-mass atmospheres are at the bottom right. Any hydrogen-rich atmospheres without high-altitude clouds, at the bottom left, are robustly ruled out. The second horizontal axis at the top shows the mean molecular mass representative for a pure H2/H2O atmosphere.
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: Generalized Lomb–Scargle (GLS) periodograms of the HARPS RV measurements (upper panel); RV residuals after subtracting the f 1 signal at 11.5 days (second panel), the f 2 signal related to stellar activity at 52.2 days (third panel), the f 3 signal at 34 days (fourth panel), and the f 4 and f 5 = f b signals at 115 days and 0.322 days (fifth panel). Also shown are periodograms of the activity indicators (remaining panels). The 10%, 1%, and 0.1% false-alarm probabilities (FAPs) estimated using the bootstrap method are shown with horizontal blue lines. The red vertical lines mark the orbital frequencies of the transiting planet GJ 367 b (f 5 = f b = 3.106 day−1), and of the additional Doppler signals we found in the HARPS data, which are associated to the presence of two additional orbiting planets (f 1 = f c = 0.086  day−1 and f 3 = f d = 0.029 day−1). The shaded yellow bands indicate the rotation period of the star centered around f 2, and the long-period stellar signal f 4.