adsabs/AstroCLIMB huggingface dataset:
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The change in magnitude vs. phase plot of GG Dra (GDR3 1425033869225305728, Gaia G magnitude 8.6141). We determined its period to be 2.2695484 days from combining TESS and our data. (a.) Our light curve points (teal) are binned (circle teal points) and folded by the period. The corresponding TESS light curves (sectors 16, 23, 25, 50, 51, 52, 77, 78, 79, and 83, black points) are included. (b.) The binary system showed no color dependence (no obvious variance in red, blue, or green data points).
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The change in magnitude vs. phase plot of GW Ursae Majoris (GW UMa, GDR3 829393545336090368, Gaia G magnitude 9.6529). We determined its period to be 0.203194 days from combining TESS and our data. Our light curve points (corresponding to each color channel (i.e., red, green, and blue)) are binned (each corresponding color channel (i.e., red, green, and blue) circle points) and folded by the period. The corresponding TESS light curves (sectors 21 and 48, black points) are included.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The scatter (median absolute deviation from the median (MAD)) of the individual channel light curves vs. GAIA G magnitude before EPD (only magnitude fitting, indicated by yellow points), after EPD but before TFA (indicated by purple points), and after TFA (indicated by their corresponding channel color (B (blue)(a), G1 (green)(b), G2 (green)(c), R (red)(d)) points). These plots are for dither pattern D26, field G111. These show the overall improvements from our postprocessing steps.
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: The scatter (median absolute deviation from the median (MAD)) of the individual channel completely processed (i.e., after performing magnitude fitting, EPD, and TFA steps) light curves vs. GAIA G magnitude, indicated by their corresponding channel color; i.e., B (blue), G1 (green), G2 (green), R (red)). These plots are for dither patterns D25 (left plots (a), (c), (e)) and D26 (right plots (b), (d), (f)), for each field G262(a, b), G111 (c, d), and G139 (e, f).
Paper: AutoWISP: Automated Processing of Wide-field Color Images 
Authors: Angel E. Romero, Kaloyan Penev, S. Javad Jafarzadeh, Zoltan Csubry, Joel D. Hartman, Gáspár 'A. Bakos
Figure caption: Similar to Figure 7, comparing the scatter of the two dither patterns, D25 (orange points) and D26 (purple points).
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Example Bioverse simulation of a survey to characterize Earth-sized planets in the HZ. This simulation used an 8 m diameter telescope observing at λ = 550 nm. This figure shows all rocky planets detected with Rp < 1.4R⊕. Left panel shows the measured quantity of β = AgR2Φ(α) as a function of instellation. Individual components of albedo, radius, and phase angle drawn from the Bioverse planet generation process including our injected trend are shown in the right subplots. This survey yields 44 exoEarth candidates, and the distribution of β shows a decrease at instellations corresponding to the HZ, reflecting the injected trend in albedo (see upper-right panel).
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Histogram of Bayes factors for random samples with 25 exoEarth candidates (EECs). Blue histogram represents points drawn from a distribution with a strong injected trend in albedo (ΔA = 0.4). Orange histogram represents points drawn from a distribution without any trend in albedo. The dashed vertical line represents the threshold for strong detection of a trend at a Bayes factor of K = 10. The region of the blue histogram to the right of this threshold represents the true-positive rate, or statistical power in favor of the albedo trend model. The region of the orange histogram to the right of the threshold represents the false-positive rate.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Survey distribution of rocky planets that would be detectable for a space-based direct imaging survey with an 8 m diameter telescope. Left panel shows the distribution of planets if there is no injected trend in albedo, while the right panel shows the case where there is a strong trend in albedo (ΔA = 0.4). This distribution was generated by simulating the output of exoEarth surveys (analogous to Figure 1) for 1000 simulated universes. Plots are color coded based on the number of recovered planets in each bin. One can clearly see the influence of population-level trends in albedo in the output, where there is a prominent dip at instellations corresponding to the HZ.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Sample size of exoEarths required to detect an injected trend in albedo. Top panels represent the true-positive rate or statistical power as a function of the sample size of exoEarths, NEEC, for two threshold values of the Bayes factor, K. Bottom subplots show the false-positive rate as a function of sample size. For each point in these subplots an analysis similar to that in Figure 3 was performed using 10,000 simulations of planetary samples at that sample size. Simulations injected a strong albedo trend with ΔA = 0.4.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: False-positive rate as a function of trend strength and sample size. Left and right subplots show results for two different threshold values for the Bayes factor required to detect an injected trend in albedo. Contours are shown for a 1% and 5% false-positive rate. Weaker trends and smaller samples of exoEarths have higher false-positive rates.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: True-positive rate as a function of trend strength, ΔA, and sample size, NEEC. Left and right subplots show results for two different threshold values for the Bayes factor required to detect an injected trend in albedo. Contours are shown for 90% and 95% statistical power. One can observe that the sample size required to detect a trend increases rapidly as the strength of the trend is reduced.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Insensitivity of the survey distribution on telescope and coronagraph parameters. Each of these scenarios take the baseline case of the survey distribution shown in Figure 2 with D = 8 m and ﹩{\mathrm{log}}\,{C}_{\min }=-10.6﹩, varying either the diameter or minimum achievable contrast. Despite second-order differences between these scenarios, they largely have the same overall shape of their survey distribution.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Comparison of kernel density estimates of the survey distribution. Left panels show a survey distribution with no injected trend, while right panels show a distribution with a strong injected trend (ΔA = 0.4). These kernel density estimates used a Gaussian kernel, changing the bandwidth parameter in each row.
Paper: Bioverse: Assessing the Ability of Direct Imaging Surveys to Empirically Constrain the Habitable Zone via Trends in Albedo
Authors: Noah W. Tuchow, Christopher C. Stark, Dániel Apai, Martin Schlecker, Kevin K. Hardegree-Ullman
Figure caption: Same as Figure 4 but demonstrating the effects of lowering the uncertainty in observed properties. Blue points are from simulations with standard uncertainty levels, while orange points have uncertainty in contrast and semimajor axis reduced by a factor of 10.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Orbit fit for HR 2562 B. The leftmost plot displays 100 randomly selected orbits, color-coded to illustrate the anticipated orbital position over time. The right panels present the measured separation and position angle as a function of time, compared to the randomly drawn orbits (in gray). Red stars represent the observations. The apparent position angle discrepancy observed between 2018 and 2020 is likely due to systematic effects inherent to GPI astrometry.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Corner plot for the orbital fit of HR 2562 B. The object demonstrates a preference for eccentric orbits less than 0.4, with the eccentricity parameter favoring values closer to circular. The semimajor axis distribution shows a prominent peak around 22 au, with no values less than 14 au. The orientation of the disk around HR 2562 B is nearly edge on, as reflected in the inclination distribution, which supports this coplanar alignment between the orbit and the disk.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Probability density distribution of the Line-of-sight stellar obliquity for YSES 1. The median obliquity is 11﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 (red dashed line), with the 16th and 84th percentiles at 3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4 and 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7 (black dotted lines), respectively.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Corner plot for the orbital fit of YSES 1 b. The object demonstrates a preference for eccentric orbits less than 0.5. The semimajor axis distribution shows a prominent peak around 146 au.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Histogram of the mutual inclination between the orbit of HR 2562 B and its disk. The distribution peaks median value of 3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩70, indicating that HR 2562 B’s orbit is nearly coplanar with the disk.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Orbit fit for YSES 1 b. See 1 for details.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Full Corner plot of HR 2562 B. The estimated posteriors are on the diagonals. The cross-sections represent the covariance with the 1, 2, and 3σ errors.
Paper: New Orbital Constraints for YSES 1 b and HR 2562 B from High-Precision Astrometry and Planetary Radial Velocities 
Authors: Jonathan Roberts, William Thompson, Jason J. Wang, Sarah Blunt, William O. Balmer, Guillaume Bourdarot, Brendan P. Bowler, Gael Chauvin, Frank Eisenhauer, Thomas K. Henning, Jens Kammerer, Flavien Kiefer, Matthew A. Kenworthy, Pierre Kervella, Sylvestre Lacour, A.-M. Lagrange, Eric L. Nielsen, Laurent Pueyo, Emily Rickman, Olli Sipilä, Silvia Spezzano, Tomas Stolker, Alice Zurlo
Figure caption: Full corner plot for the orbital fit of YSES 1 b.
Paper: The MiMO Catalog: Physical Parameters and Stellar Mass Functions of 1232 Open Clusters from Gaia DR3
Authors: Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Zhaozhou Li, 昭洲 李, Xiaoting Fu, 晓婷 符
Figure caption: Illustration of MiMO on OCs with different data quality. The color bar shows the photometric membership probability for individual stars. The left panels show high-quality clusters (named as “MF-prime”) with clear and thin main sequences, while the middle panels represent typical cases with moderate main-sequence broadening. The right panels display clusters where MiMO failed to fit a reasonable isochrone due to extreme field-star contamination. In each panel, gray dots represent the accessory star sample used to construct the nonparametric field-star model, and the orange line indicates the best-fit isochrone from MiMO.
Paper: The MiMO Catalog: Physical Parameters and Stellar Mass Functions of 1232 Open Clusters from Gaia DR3
Authors: Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Zhaozhou Li, 昭洲 李, Xiaoting Fu, 晓婷 符
Figure caption: Distributions of formal uncertainties for parameters of OCs in our catalog, as inferred by MiMO. For reference, the uncertainty distributions from the D21 catalog are also shown when applicable.
Paper: The MiMO Catalog: Physical Parameters and Stellar Mass Functions of 1232 Open Clusters from Gaia DR3
Authors: Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Zhaozhou Li, 昭洲 李, Xiaoting Fu, 晓婷 符
Figure caption: Parameter distributions of OCs in the catalog, for the full catalog and MF-prime samples, respectively.
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Comparison of results from the PICASO grid and free-retrieval atmospheric modeling. Colored lines show abundance profiles from the PICASO grid as a function of pressure: solid for chemical equilibrium, dotted for models including photochemistry. The shaded 2σ regions represent the credible intervals of the vertical mixing ratio profiles from the grid-retrieval across the PICASO model grid. Posterior distributions from the free retrievals are shown as histograms; while plotted at the bottom of the panels for clarity, they represent average abundances primarily constrained between ∼ 10−2 and 10−4 bar. The gray horizontal line indicates the free-retrieval best-fit cloud top pressure. Left: carbon-bearing species and H2O. Right: sulfur-bearing species. For log(H2S), we show posteriors from models with (filled) and without (unfilled) a fitted NRS1–NRS2 offset.
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Predicted average SO2 volume mixing ratio (VMR) at 10−3 bar, as a function of increasing elemental abundance in log space from I. J. M. Crossfield (2023) (dashed black line), overplotted with JWST measurements from published transmission spectra of giant planets. SO2 abundances and metallicities are taken from the literature. When SO2 is not detected, 3σ upper limits are shown. When metallicity is not provided, a 3σ upper limit is derived from a free retrieval using TauREx, following a setup similar to that described in Table A1. References: GJ 1214b: E. Schlawin et al. (2024) and K. Ohno et al. (2025); GJ 3470b: T. G. Beatty et al. (2024); HAT-P-26 b: this work; HD 189733b: G. Fu et al. (2024); HD 209458b: Q. Xue et al. (2024); HIP 67522b: P. C. Thao et al. (2024); WASP-107 b: D. K. Sing et al. (2024); WASP-121 b: G. Fu et al. (2025) and this work; WASP-127 b: G. Fu et al. (2025) and this work; WASP-39 b: L. Alderson et al. (2023); WASP-80 b: T. J. Bell et al. (2023) .
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Two independent reductions of the HAT-P-26 b NIRSpec G395H transit observations. Top: transmission spectra from the transitspectroscopy (magenta) and ExoTiC-JEDI (dark cyan) pipelines, with 1σ uncertainties binned to a resolving power R ∼ 400. These data are available in machine-readable format in a .tar.gz package. Bottom: residuals (in ppm) between the transitspectroscopy and ExoTiC-JEDI transmission spectra. The two data reduction agree at 1σ and show a similar shape. The transitspectroscopy spectrum exhibits larger dispersion and uncertainties, due to the use of Gaussian Process detrending in the light-curve fits.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Posterior distributions for the free retrievals of the JWST NIRSpec G395H transmission spectrum of HAT-P-26 b, based on the transitspectroscopy reduction. The different colors correspond to the various retrieval setups described in Table A1. The retrieved values shown correspond to the best-fitting parameters from the POSEIDONTLS setup (blue).
Paper: JWST-TST DREAMS: Sulfur Dioxide in the Atmosphere of the Neptune-mass Planet HAT-P-26 b from NIRSpec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Natasha E. Batalha, Nicholas Wogan, Lili Alderson, Dominic Doud, Néstor Espinoza, Ryan J. MacDonald, Hannah R. Wakeford, Jeff A. Valenti, Nikole K. Lewis, Sara Seager, Kevin B. Stevenson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Ana Glidden, Jingcheng Huang, Zifan Lin, Dana R. Louie, Cathal Maguire, Elijah Mullens, Kristin Sotzen, Daniel Valentine, Mark Clampin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Spectroscopic and broadband light curves for the JWST NIRSpec G395H transit observation of HAT-P-26 b. Top: raw spectroscopic light curves for NRS1 and NRS2 from the transitspectroscopy reduction. Middle: detrended broadband light curves with the best-fit transit model shown in black. These data are available in machine-readable format in a .tar.gz package. Bottom: residuals between the broadband light curves and the best-fit model. Data points at full temporal resolution are shown in purple (NRS1) and blue (NRS2) with their associated uncertainties. White data points represent time-binned data for clarity.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)